{"id":1113,"date":"2018-02-06T17:25:46","date_gmt":"2018-02-06T17:25:46","guid":{"rendered":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/?post_type=chapter&#038;p=1113"},"modified":"2019-01-17T18:35:18","modified_gmt":"2019-01-17T18:35:18","slug":"13-1-newtons-law-of-universal-gravitation","status":"publish","type":"chapter","link":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/chapter\/13-1-newtons-law-of-universal-gravitation\/","title":{"raw":"13.1 Newton\u2019s Law of Universal Gravitation","rendered":"13.1 Newton\u2019s Law of Universal Gravitation"},"content":{"raw":"<div class=\"textbox learning-objectives\">\r\n<h3>Learning Objectives<\/h3>\r\nBy the end of this section, you will be able to:\r\n<ul>\r\n \t<li>List the significant milestones in the history of gravitation<\/li>\r\n \t<li>Calculate the gravitational force between two point masses<\/li>\r\n \t<li>Estimate the gravitational force between collections of mass<\/li>\r\n<\/ul>\r\n<\/div>\r\n<p id=\"fs-id1168327959267\">We first review the history of the study of gravitation, with emphasis on those phenomena that for thousands of years have inspired philosophers and scientists to search for an explanation. Then we examine the simplest form of Newton\u2019s law of universal gravitation and how to apply it.<\/p>\r\n\r\n<div id=\"fs-id1168327975150\" class=\"bc-section section\">\r\n<h3>The History of Gravitation<\/h3>\r\n<p id=\"fs-id1168325664369\">The earliest philosophers wondered why objects naturally tend to fall toward the ground. Aristotle (384\u2013322 BCE) believed that it was the nature of rocks to seek Earth and the nature of fire to seek the Heavens. Brahmagupta (598~665 CE) postulated that Earth was a sphere and that objects possessed a natural affinity for it, falling toward the center from wherever they were located.<\/p>\r\nThe motions of the Sun, our Moon, and the planets have been studied for thousands of years as well. These motions were described with amazing accuracy by <strong><span class=\"no-emphasis\">Ptolemy<\/span><\/strong> (90\u2013168 CE), whose method of epicycles described the paths of the planets as circles within circles. However, there is little evidence that anyone connected the motion of astronomical bodies with the motion of objects falling to Earth\u2014until the seventeenth century.\r\n<p id=\"fs-id1168328266543\">Nicolaus <strong><span class=\"no-emphasis\">Copernicus<\/span><\/strong> (1473\u20131543) is generally credited as being the first to challenge Ptolemy\u2019s geocentric (Earth-centered) system and suggest a heliocentric system, in which the Sun is at the center of the solar system. This idea was supported by the incredibly precise naked-eye measurements of planetary motions by Tycho <strong><span class=\"no-emphasis\">Brahe<\/span><\/strong> and their analysis by Johannes <strong><span class=\"no-emphasis\">Kepler<\/span><\/strong> and <strong><span class=\"no-emphasis\">Galileo<\/span><\/strong> Galilei. Kepler showed that the motion of each planet is an ellipse (the first of his three laws, discussed in <a class=\"target-chapter\" href=\"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/chapter\/13-5-keplers-laws-of-planetary-motion\/\">Kepler\u2019s Laws of Planetary Motion<\/a>), and Robert Hooke (the same Hooke who formulated Hooke\u2019s law for springs) intuitively suggested that these motions are due to the planets being attracted to the Sun. However, it was Isaac Newton who connected the acceleration of objects near Earth\u2019s surface with the centripetal acceleration of the Moon in its orbit about Earth.<\/p>\r\n<p id=\"fs-id1168328256234\">Finally, in <a class=\"target-chapter\" href=\"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/chapter\/13-8-einsteins-theory-of-gravity\/\">Einstein\u2019s Theory of Gravity<\/a>, we look at the theory of general relativity proposed by Albert Einstein in 1916. His theory comes from a vastly different perspective, in which gravity is a manifestation of mass warping space and time. The consequences of his theory gave rise to many remarkable predictions, essentially all of which have been confirmed over the many decades following the publication of the theory (including the 2015 measurement of gravitational waves from the merger of two black holes).<\/p>\r\n\r\n<\/div>\r\n<div id=\"fs-id1168327958865\" class=\"bc-section section\">\r\n<h3>Newton\u2019s Law of Universal Gravitation<\/h3>\r\n<p id=\"fs-id1168327941709\"><strong><span class=\"no-emphasis\">Newton<\/span><\/strong> noted that objects at Earth\u2019s surface (hence at a distance of $$ {R}_{\\text{E}} $$ from the center of Earth) have an acceleration of <em>g<\/em>, but the Moon, at a distance of about $$ 60\\,{R}_{\\text{E}}$$, has a centripetal acceleration about $$ {(60)}^{2} $$ times smaller than <em>g<\/em>. He could explain this by postulating that a force exists between any two objects, whose magnitude is given by the product of the two masses divided by the square of the distance between them. We now know that this inverse square law is ubiquitous in nature, a function of geometry for point sources. The strength of any source at a distance <em>r<\/em> is spread over the surface of a sphere centered about the mass. The surface area of that sphere is proportional to $$ {r}^{2}$$. In later chapters, we see this same form in the electromagnetic force.<\/p>\r\n\r\n<div id=\"fs-id1168325679209\">\r\n<h4>Newton\u2019s Law of Gravitation<\/h4>\r\n<p id=\"fs-id1168325728231\">Newton\u2019s law of gravitation can be expressed as<\/p>\r\n\r\n<div id=\"fs-id1168327894017\"><a id=\"eq13.1\"><\/a>$${\\overset{\\to }{F}}_{12}=G\\frac{{m}_{1}{m}_{2}}{{r}^{2}}{\\hat{r}}_{12}$$<\/div>\r\n<p id=\"fs-id1168328260151\">where $$ {\\overset{\\to }{F}}_{12} $$ is the force on object 1 exerted by object 2 and $$ {\\hat{r}}_{12} $$ is a unit vector that points from object 1 toward object 2.<\/p>\r\n\r\n<\/div>\r\n<p id=\"fs-id1168328167966\">As shown in <a class=\"autogenerated-content\" href=\"#CNX_UPhysics_13_01_NewtonLofG\">(Figure)<\/a>, the $$ {\\overset{\\to }{F}}_{12} $$ vector points from object 1 toward object 2, and hence represents an attractive force between the objects. The equal but opposite force $$ {\\overset{\\to }{F}}_{21} $$ is the force on object 2 exerted by object 1.<\/p>\r\n\r\n<div id=\"CNX_UPhysics_13_01_NewtonLofG\" class=\"wp-caption aligncenter\">\r\n\r\n[caption id=\"\" align=\"aligncenter\" width=\"430\"]<img src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195821\/CNX_UPhysics_13_01_NewtonLofG.jpg\" alt=\"The figure shows two circular objects, one smaller, labeled as mass m1 on the lower left, and the larger one labeled m2 on the upper right. The center of each object is labeled C M. A line is drawn joining the center of the objects and is labeled as r. Two red arrows and two black arrows, one each from the center of each object, are drawn toward each other. The black arrow from the center of mass 1 is labeled r hat 1 2 and the red arrow from mass 1 is labeled F 1 2. The black arrow from the center of mass 2 is labeled r hat 2 1 and the red arrow from mass 2 is labeled F 2 1.\" width=\"430\" height=\"343\" \/> <strong>Figure 13.2<\/strong> Gravitational force acts along a line joining the centers of mass of two objects.[\/caption]\r\n\r\n<\/div>\r\n<p id=\"fs-id1168328271118\">These equal but opposite forces reflect Newton\u2019s third law, which we discussed earlier. Note that strictly speaking, <a class=\"autogenerated-content\" href=\"#fs-id1168327894017\">(Figure)<\/a> applies to point masses\u2014all the mass is located at one point. But it applies equally to any spherically symmetric objects, where <em>r<\/em> is the distance between the centers of mass of those objects. In many cases, it works reasonably well for nonsymmetrical objects, if their separation is large compared to their size, and we take <em>r<\/em> to be the distance between the center of mass of each body.<\/p>\r\n\r\n<\/div>\r\n<div id=\"fs-id1168328373219\" class=\"bc-section section\">\r\n<h3>The Cavendish Experiment<\/h3>\r\n<p id=\"fs-id1168328366420\">A century after Newton published his law of universal gravitation, Henry <strong><span class=\"no-emphasis\">Cavendish<\/span><\/strong> determined the proportionality constant <em>G<\/em> by performing a painstaking experiment. He constructed a device similar to that shown in <a class=\"autogenerated-content\" href=\"#CNX_UPhysics_13_01_Cavendish\">(Figure)<\/a>, in which small masses are suspended from a wire. Once in equilibrium, two fixed, larger masses are placed symmetrically near the smaller ones. The gravitational attraction creates a torsion (twisting) in the supporting wire that can be measured.<\/p>\r\n<p id=\"fs-id1168325860685\">The constant <em>G<\/em> is called the<strong> universal gravitational constant<\/strong> and Cavendish determined it to be $$ G=6.67\\,\u00d7\\,{10}^{-11}\\,\\text{N}\u00b7{\\text{m}}^{2}{\\text{\/kg}}^{2}$$. The word \u2018universal\u2019 indicates that scientists think that this constant applies to masses of any composition and that it is the same throughout the Universe. The value of <em>G<\/em> is an incredibly small number, showing that the force of gravity is very weak. The attraction between masses as small as our bodies, or even objects the size of skyscrapers, is incredibly small. For example, two 1.0-kg masses located 1.0 meter apart exert a force of $$ 6.7\\,\u00d7\\,{10}^{-11}\\,\\text{N} $$ on each other. This is the weight of a typical grain of pollen.<\/p>\r\n\r\n<div id=\"CNX_UPhysics_13_01_Cavendish\" class=\"wp-caption aligncenter\">\r\n\r\n[caption id=\"\" align=\"aligncenter\" width=\"566\"]<img src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195824\/CNX_UPhysics_13_01_Cavendish.jpg\" alt=\"The figure illustrates the Cavendish experiment. A horizontal bar, centered on a stand, supports two spheres of mass M, one at either of its ends. The point where the bar sits on the stand is labeled &quot;pivot&quot;. Just over this bar is a stick holding two spherical objects of mass m, one mass at either of its ends. This bar is suspended from a mirror at the center of the device facing to the right. The mirror is suspended from a fiber. The rotation of the fiber over the axis of the stand is counter-clockwise. A light source on the right side of the device emits a ray of light toward the mirror which is then reflected toward a scale bar which is on the right to the device below the light source.\" width=\"566\" height=\"495\" \/> <strong>Figure 13.3<\/strong> Cavendish used an apparatus similar to this to measure the gravitational attraction between two spheres (m) suspended from a wire and two stationary spheres (M). This is a common experiment performed in undergraduate laboratories, but it is quite challenging. Passing trucks outside the laboratory can create vibrations that overwhelm the gravitational forces.[\/caption]\r\n\r\n<\/div>\r\n<p id=\"fs-id1168328290504\">Although gravity is the weakest of the four fundamental forces of nature, its attractive nature is what holds us to Earth, causes the planets to orbit the Sun and the Sun to orbit our galaxy, and binds galaxies into clusters, ranging from a few to millions. Gravity is the force that forms the Universe.<\/p>\r\n\r\n<div id=\"fs-id1168328307578\" class=\"problem-solving\">\r\n<h4>Problem-Solving Strategy: Newton\u2019s Law of Gravitation<\/h4>\r\n<p id=\"fs-id1168327922730\">To determine the motion caused by the gravitational force, follow these steps:<\/p>\r\n\r\n<ol id=\"fs-id1168328303662\" type=\"1\">\r\n \t<li>Identify the two masses, one or both, for which you wish to find the gravitational force.<\/li>\r\n \t<li>Draw a free-body diagram, sketching the force acting on each mass and indicating the distance between their centers of mass.<\/li>\r\n \t<li>Apply Newton\u2019s second law of motion to each mass to determine how it will move.<\/li>\r\n<\/ol>\r\n<\/div>\r\n<div id=\"fs-id1168328269876\" class=\"textbox examples\">\r\n<h3>Example<\/h3>\r\n<h4>A Collision in Orbit<\/h4>\r\nConsider two nearly spherical <em>Soyuz<\/em> payload vehicles, in orbit about Earth, each with mass 9000 kg and diameter 4.0 m. They are initially at rest relative to each other, 10.0 m from center to center. (As we will see in <a class=\"target-chapter\" href=\"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/chapter\/13-5-keplers-laws-of-planetary-motion\/\">Kepler\u2019s Laws of Planetary Motion<\/a>, both orbit Earth at the same speed and interact nearly the same as if they were isolated in deep space.) Determine the gravitational force between them and their initial acceleration. Estimate how long it takes for them to drift together, and how fast they are moving upon impact.\r\n<h4>Strategy<\/h4>\r\nWe use Newton\u2019s law of gravitation to determine the force between them and then use Newton\u2019s second law to find the acceleration of each. For the <em>estimate<\/em>, we assume this acceleration is constant, and we use the constant-acceleration equations from <a class=\"target-chapter\" href=\"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/chapter\/introduction-3\/\">Motion along a Straight Line<\/a> to find the time and speed of the collision.\r\n<h4>Solution<\/h4>\r\n<p id=\"fs-id1168325735813\">The magnitude of the force is<\/p>\r\n\r\n<div id=\"fs-id1168056388170\" class=\"unnumbered\">$$|{\\overset{\\to }{F}}_{12}|={F}_{12}=G\\,\\frac{{m}_{1}{m}_{2}}{{r}^{2}}=6.67\\,\u00d7\\,{10}^{-11}\\,\\text{N}\u00b7{\\text{m}}^{2}{\\text{\/kg}}^{2}\\frac{(9000\\,\\text{kg})(9000\\,\\text{kg})}{{(10\\,\\text{m})}^{2}}=5.4\\,\u00d7\\,{10}^{-5}\\text{N.}$$<\/div>\r\n<p id=\"fs-id1168327940864\">The initial acceleration of each payload is<\/p>\r\n\r\n<div id=\"fs-id1168056081366\" class=\"unnumbered\">$$a=\\frac{F}{m}=\\frac{5.4\\,\u00d7\\,{10}^{-5}\\,\\text{N}}{9000\\,\\text{kg}}=6.0\\,\u00d7\\,{10}^{-9}{\\text{m\/s}}^{2}.$$<\/div>\r\n<p id=\"fs-id1168328379763\">The vehicles are 4.0 m in diameter, so the vehicles move from 10.0 m to 4.0 m apart, or a distance of 3.0 m each. A similar calculation to that above, for when the vehicles are 4.0 m apart, yields an acceleration of $$ 3.8\\,\u00d7\\,{10}^{-8}\\,{\\text{m\/s}}^{2}$$, and the average of these two values is $$ 2.2\\,\u00d7\\,{10}^{-8}\\,{\\text{m\/s}}^{2}$$. If we assume a constant acceleration of this value and they start from rest, then the vehicles collide with speed given by<\/p>\r\n\r\n<div id=\"fs-id1168056179542\" class=\"unnumbered\">$${v}^{2}={v}_{0}^{2}+2a(x-{x}_{0}),\\,\\text{where}\\,{v}_{0}=0,$$<\/div>\r\n<p id=\"fs-id1168327886813\">so<\/p>\r\n\r\n<div id=\"fs-id1168056221144\" class=\"unnumbered\">$$v=\\sqrt{2(2.2\\,\u00d7\\,{10}^{-9}\\,\\text{N})(3.0\\,\\text{m})}=3.6\\,\u00d7\\,{10}^{-4}\\,\\,\\text{m\/s.}$$<\/div>\r\n<p id=\"fs-id1168328173465\">We use $$ {v}^{}={v}_{0}+at $$ to find $$ t=v\\text{\/}a=1.7\\,\u00d7\\,{10}^{4}\\,\\text{s} $$ or about 4.6 hours.<\/p>\r\n\r\n<h4>Significance<\/h4>\r\nThese calculations\u2014including the initial force\u2014are only estimates, as the vehicles are probably not spherically symmetrical. But you can see that the force is incredibly small. Astronauts must tether themselves when doing work outside even the massive International Space Station (ISS), as in <a class=\"autogenerated-content\" href=\"#CNX_UPhysics_13_01_Spacewalk\">(Figure)<\/a>, because the gravitational attraction cannot save them from even the smallest push away from the station.\r\n<div id=\"CNX_UPhysics_13_01_Spacewalk\" class=\"wp-caption aligncenter\">\r\n\r\n[caption id=\"\" align=\"aligncenter\" width=\"488\"]<img src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195829\/CNX_UPhysics_13_01_Spacewalk.jpg\" alt=\"A photo of an astronaut on a spacewalk is shown.\" width=\"488\" height=\"489\" \/> <strong>Figure 13.4<\/strong> This photo shows Ed White tethered to the Space Shuttle during a spacewalk. (credit: NASA)[\/caption]\r\n\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168328230996\" class=\"textbox exercises check-understanding\">\r\n<h3>Check Your Understanding<\/h3>\r\n<div id=\"fs-id1168327958408\" class=\"problem textbox\">\r\n<div id=\"fs-id1168328367049\">\r\n<p id=\"fs-id1168327870892\">What happens to force and acceleration as the vehicles fall together? What will our estimate of the velocity at a collision higher or lower than the speed actually be? And finally, what would happen if the masses were not identical? Would the force on each be the same or different? How about their accelerations?<\/p>\r\n\r\n<\/div>\r\n<div id=\"fs-id1168327933345\" class=\"solution\">\r\n\r\n[reveal-answer q=\"fs-id1168327933345\"]Show Solution[\/reveal-answer]\r\n\r\n[hidden-answer a=\"fs-id1168327933345\"]\r\n<p id=\"fs-id1168328312328\">The force of gravity on each object increases with the square of the inverse distance as they fall together, and hence so does the acceleration. For example, if the distance is halved, the force and acceleration are quadrupled. Our average is accurate only for a linearly increasing acceleration, whereas the acceleration actually increases at a greater rate. So our calculated speed is too small. From Newton\u2019s third law (action-reaction forces), the force of gravity between any two objects must be the same. But the accelerations will not be if they have different masses.<\/p>\r\n[\/hidden-answer]\r\n\r\n<\/div>\r\n<\/div>\r\n<\/div>\r\n<p id=\"fs-id1168328270037\">The effect of gravity between two objects with masses on the order of these space vehicles is indeed small. Yet, the effect of gravity on you from Earth is significant enough that a fall into Earth of only a few feet can be dangerous. We examine the force of gravity near Earth\u2019s surface in the next section.<\/p>\r\n\r\n<div id=\"fs-id1168327873949\" class=\"textbox examples\">\r\n<h3>Example<\/h3>\r\n<h4>Attraction between Galaxies<\/h4>\r\nFind the acceleration of our galaxy, the <strong><span class=\"no-emphasis\">Milky Way<\/span><\/strong>, due to the nearest comparably sized galaxy, the <strong><span class=\"no-emphasis\">Andromeda galaxy<\/span><\/strong> (<a class=\"autogenerated-content\" href=\"#CNX_UPhysics_13_01_Androm\">(Figure)<\/a>). The approximate mass of each galaxy is 800 billion solar masses (a solar mass is the mass of our Sun), and they are separated by 2.5 million light-years. (Note that the mass of Andromeda is not so well known but is believed to be slightly larger than our galaxy.) Each galaxy has a diameter of roughly 100,000 light-years $$ (1\\,\\text{light-year}=9.5\\,\u00d7\\,{10}^{15}\\,\\,\\text{m})$$.\r\n<div id=\"CNX_UPhysics_13_01_Androm\" class=\"wp-caption aligncenter\">\r\n\r\n[caption id=\"\" align=\"aligncenter\" width=\"731\"]<img src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195834\/CNX_UPhysics_13_01_Androm.jpg\" alt=\"A photograph of the Andromeda galaxy is shown.\" width=\"731\" height=\"491\" \/> <strong>Figure 13.5<\/strong> Galaxies interact gravitationally over immense distances. The Andromeda galaxy is the nearest spiral galaxy to the Milky Way, and they will eventually collide. (credit: Boris \u0160tromar)[\/caption]\r\n\r\n<\/div>\r\n<h4>Strategy<\/h4>\r\nAs in the preceding example, we use Newton\u2019s law of gravitation to determine the force between them and then use Newton\u2019s second law to find the acceleration of the Milky Way. We can consider the galaxies to be point masses, since their sizes are about 25 times smaller than their separation. The mass of the Sun (see <a class=\"target-chapter\" href=\"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/back-matter\/astronomical-data\/\">Appendix D<\/a>) is $$ 2.0\\,\u00d7\\,{10}^{30}\\,\\text{kg} $$ and a light-year is the distance light travels in one year, $$ 9.5\\,\u00d7\\,{10}^{15}\\,\\text{m}$$.\r\n<h4>Solution<\/h4>\r\n<p id=\"fs-id1168328323842\">The magnitude of the force is<\/p>\r\n\r\n<div id=\"fs-id1168056208576\" class=\"unnumbered\">$${F}_{12}=G\\,\\frac{{m}_{1}{m}_{2}}{{r}^{2}}=(6.67\\,\u00d7\\,{10}^{-11}\\,\\text{N}\u00b7{\\text{m}}^{2}\\text{\/}{\\text{kg}}^{2})\\frac{{[(800\\,\u00d7\\,{10}^{9})(2.0\\,\u00d7\\,{10}^{30}\\,\\text{kg})]}^{2}}{{[(2.5\\,\u00d7\\,{10}^{6})(9.5\\,\u00d7\\,{10}^{15}\\,\\text{m})]}^{2}}=3.0\\,\u00d7\\,{10}^{29}\\,\\text{N.}$$<\/div>\r\n<p id=\"fs-id1168327874267\">The acceleration of the Milky Way is<\/p>\r\n\r\n<div id=\"fs-id1168056218734\" class=\"unnumbered\">$$a=\\frac{F}{m}=\\frac{3.0\\,\u00d7\\,{10}^{29}\\,\\text{N}}{(800\\,\u00d7\\,{10}^{9})(2.0\\,\u00d7\\,{10}^{30}\\,\\text{kg})}=1.9\\,\u00d7\\,{10}^{-13}{\\text{m\/s}}^{2}.$$<\/div>\r\n<h4>Significance<\/h4>\r\nDoes this value of acceleration seem astoundingly small? If they start from rest, then they would accelerate directly toward each other, \u201ccolliding\u201d at their center of mass. Let\u2019s estimate the time for this to happen. The initial acceleration is $$ ~{10}^{-13}\\,{\\text{m\/s}}^{2}$$, so using $$ v=at$$, we see that it would take $$ ~{10}^{13}\\,\\text{s} $$ for each galaxy to reach a speed of 1.0 m\/s, and they would be only $$ ~0.5\\,\u00d7\\,{10}^{13}\\,\\text{m} $$ closer. That is nine orders of magnitude smaller than the initial distance between them. In reality, such motions are rarely simple. These two galaxies, along with about 50 other smaller galaxies, are all gravitationally bound into our local cluster. Our local cluster is gravitationally bound to other clusters in what is called a supercluster. All of this is part of the great cosmic dance that results from gravitation, as shown in <a class=\"autogenerated-content\" href=\"#CNX_UPhysics_13_01_Collide\">(Figure)<\/a>.\r\n<div id=\"CNX_UPhysics_13_01_Collide\" class=\"wp-caption aligncenter\">\r\n\r\n[caption id=\"\" align=\"aligncenter\" width=\"900\"]<img src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195841\/CNX_UPhysics_13_01_Collide.jpg\" alt=\"An illustration of the Milky Way galaxy, the Andromeda galaxy (M31), shown above and to the left of the Milky Way, and the Triangulum galaxy (M33) shown above the Andromeda galaxy. The sun is labeled in the Milky way. Arrows pointing from the Milky way toward Andromeda and from Andromeda to the Milky way meet between the two galaxies and are labeled &quot;collision in 4 billion years.&quot;\" width=\"900\" height=\"599\" \/> <strong>Figure 13.6<\/strong> Based on the results of this example, plus what astronomers have observed elsewhere in the Universe, our galaxy will collide with the Andromeda Galaxy in about 4 billion years. (credit: NASA)[\/caption]\r\n\r\n<\/div>\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168327911320\" class=\"textbox key-takeaways\">\r\n<h3>Summary<\/h3>\r\n<ul id=\"fs-id1168328367162\">\r\n \t<li>All masses attract one another with a gravitational force proportional to their masses and inversely proportional to the square of the distance between them.<\/li>\r\n \t<li>Spherically symmetrical masses can be treated as if all their mass were located at the center.<\/li>\r\n \t<li>Nonsymmetrical objects can be treated as if their mass were concentrated at their center of mass, provided their distance from other masses is large compared to their size.<\/li>\r\n<\/ul>\r\n<\/div>\r\n<div id=\"fs-id1168327940992\" class=\"review-conceptual-questions\">\r\n<h3>Conceptual Questions<\/h3>\r\n<div id=\"fs-id1168328367169\" class=\"problem textbox\">\r\n<div id=\"fs-id1168327949431\">\r\n<p id=\"fs-id1168327949433\">Action at a distance, such as is the case for gravity, was once thought to be illogical and therefore untrue. What is the ultimate determinant of the truth in science, and why was this action at a distance ultimately accepted?<\/p>\r\n\r\n<\/div>\r\n<div id=\"fs-id1168328304318\" class=\"solution\">\r\n\r\n[reveal-answer q=\"fs-id1168328304318\"]Show Solution[\/reveal-answer]\r\n\r\n[hidden-answer a=\"fs-id1168328304318\"]\r\n<p id=\"fs-id1168328304320\">The ultimate truth is experimental verification. Field theory was developed to help explain how force is exerted without objects being in contact for both gravity and electromagnetic forces that act at the speed of light. It has only been since the twentieth century that we have been able to measure that the force is not conveyed immediately.<\/p>\r\n[\/hidden-answer]\r\n\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168325860246\" class=\"problem textbox\">\r\n<div id=\"fs-id1168328371916\">\r\n<p id=\"fs-id1168328371918\">In the law of universal gravitation, Newton assumed that the force was proportional to the product of the two masses ($$~{m}_{1}{m}_{2}$$). While all scientific conjectures must be experimentally verified, can you provide arguments as to why this must be? (You may wish to consider simple examples in which any other form would lead to contradictory results.)<\/p>\r\n\r\n<\/div>\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168327952737\" class=\"review-problems textbox exercises\">\r\n<h3>Problems<\/h3>\r\n<div id=\"fs-id1168328366602\" class=\"problem textbox\">\r\n<div id=\"fs-id1168328366604\">\r\n<p id=\"fs-id1168328238746\">Evaluate the magnitude of gravitational force between two 5-kg spherical steel balls separated by a center-to-center distance of 15 cm.<\/p>\r\n\r\n<\/div>\r\n<div id=\"fs-id1168325667098\" class=\"solution\">\r\n\r\n[reveal-answer q=\"fs-id1168325667098\"]Show Solution[\/reveal-answer]\r\n\r\n[hidden-answer a=\"fs-id1168325667098\"]\r\n<p id=\"fs-id1168325667100\">$$7.4\\,\u00d7\\,{10}^{-8}\\,\\text{N}$$<\/p>\r\n[\/hidden-answer]\r\n\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168328379314\" class=\"problem textbox\">\r\n<div id=\"fs-id1168328379316\">\r\n<p id=\"fs-id1168328379318\">Estimate the gravitational force between two sumo wrestlers, with masses 220 kg and 240 kg, when they are embraced and their centers are 1.2 m apart.<\/p>\r\n\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168328199977\" class=\"problem textbox\">\r\n<div id=\"fs-id1168328199979\">\r\n<p id=\"fs-id1168325664395\">Astrology makes much of the position of the planets at the moment of one\u2019s birth. The only known force a planet exerts on Earth is gravitational. (a) Calculate the gravitational force exerted on a 4.20-kg baby by a 100-kg father 0.200 m away at birth (he is assisting, so he is close to the child). (b) Calculate the force on the baby due to Jupiter if it is at its closest distance to Earth, some $$ 6.29\\,\u00d7\\,{10}^{11}\\,\\text{m} $$ away. How does the force of Jupiter on the baby compare to the force of the father on the baby? Other objects in the room and the hospital building also exert similar gravitational forces. (Of course, there could be an unknown force acting, but scientists first need to be convinced that there is even an effect, much less that an unknown force causes it.)<\/p>\r\n\r\n<\/div>\r\n<div id=\"fs-id1168328070155\" class=\"solution\">\r\n\r\n[reveal-answer q=\"fs-id1168328070155\"]Show Solution[\/reveal-answer]\r\n\r\n[hidden-answer a=\"fs-id1168328070155\"]\r\n<p id=\"fs-id1168328070157\">a. $$ 7.01\\,\u00d7\\,{10}^{-7}\\,\\text{N}$$; b. The mass of Jupiter is<\/p>\r\n$$\\begin{array}{cc} {m}_{\\text{J}}=1.90\\,\u00d7\\,{10}^{27}\\,\\text{kg}\\hfill \\\\ {F}_{\\text{J}}=1.35\\,\u00d7\\,{10}^{-6}\\,\\text{N}\\hfill \\\\ \\frac{{F}_{\\text{f}}}{{F}_{\\text{J}}}=0.521\\hfill \\end{array}$$[\/hidden-answer]\r\n\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168328170296\" class=\"problem textbox\">\r\n<div id=\"fs-id1168328170298\">\r\n<p id=\"fs-id1168328170300\">A mountain 10.0 km from a person exerts a gravitational force on him equal to 2.00% of his weight. (a) Calculate the mass of the mountain. (b) Compare the mountain\u2019s mass with that of Earth. (c) What is unreasonable about these results? (d) Which premises are unreasonable or inconsistent? (Note that accurate gravitational measurements can easily detect the effect of nearby mountains and variations in local geology.)<\/p>\r\n\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168327953090\" class=\"problem textbox\">\r\n<div id=\"fs-id1168328281975\">\r\n<p id=\"fs-id1168328281977\">The International Space Station has a mass of approximately 370,000 kg. (a) What is the force on a 150-kg suited astronaut if she is 20 m from the center of mass of the station? (b) How accurate do you think your answer would be?<\/p>\r\n\r\n<div id=\"CNX_UPhysics_13_01_ISS_img\" class=\"wp-caption aligncenter\">\r\n\r\n[caption id=\"\" align=\"aligncenter\" width=\"450\"]<img src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195846\/CNX_UPhysics_13_01_ISS_img.jpg\" alt=\"An image of the international space station is shown.\" width=\"450\" height=\"360\" \/> <strong>Figure 13.33<\/strong> (credit: \u00a9ESA\u2013David Ducros)[\/caption]\r\n\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168328358280\">\r\n\r\n[reveal-answer q=\"496557\"]Show Solution[\/reveal-answer]\r\n[hidden-answer a=\"496557\"]a. $$ 9.25\\,\u00d7\\,{10}^{-6}\\,\\text{N}$$; b. Not very, as the ISS is not even symmetrical, much less spherically symmetrical.[\/hidden-answer]\r\n\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168327933478\" class=\"problem textbox\">\r\n<div id=\"fs-id1168327885276\">\r\n<p id=\"fs-id1168327885278\">Asteroid Toutatis passed near Earth in 2006 at four times the distance to our Moon. This was the closest approach we will have until 2060. If it has mass of $$ 5.0\\,\u00d7\\,{10}^{13}\\,\\text{kg}$$, what force did it exert on Earth at its closest approach?<\/p>\r\n\r\n<\/div>\r\n<\/div>\r\n<div id=\"fs-id1168328367241\" class=\"problem textbox\">\r\n<div id=\"fs-id1168327885649\">\r\n<p id=\"fs-id1168327885651\">(a) What was the acceleration of Earth caused by asteroid Toutatis (see previous problem) at its closest approach? (b) What was the acceleration of Toutatis at this point?<\/p>\r\n\r\n<\/div>\r\n<div id=\"fs-id1168327911238\" class=\"solution\">\r\n\r\n[reveal-answer q=\"fs-id1168327911238\"]Show Solution[\/reveal-answer]\r\n\r\n[hidden-answer a=\"fs-id1168327911238\"]\r\n<p id=\"fs-id1168327885653\">a. $$ 1.41\\,\u00d7\\,{10}^{-15}{\\text{m\/s}}^{2}$$; b. $$ 1.69\\,\u00d7\\,{10}^{-4}\\,{\\text{m\/s}}^{2}$$<\/p>\r\n[\/hidden-answer]\r\n\r\n<\/div>\r\n<\/div>\r\n<\/div>\r\n<div class=\"textbox shaded\">\r\n<h3>Glossary<\/h3>\r\n<dl id=\"fs-id1168328193986\">\r\n \t<dt><strong>Newton\u2019s law of gravitation<\/strong><\/dt>\r\n \t<dd id=\"fs-id1168327988168\">every mass attracts every other mass with a force proportional to the product of their masses, inversely proportional to the square of the distance between them, and with direction along the line connecting the center of mass of each<\/dd>\r\n<\/dl>\r\n<dl id=\"fs-id1168328252700\">\r\n \t<dt><strong>universal gravitational constant<\/strong><\/dt>\r\n \t<dd id=\"fs-id1168328252706\">constant representing the strength of the gravitational force, that is believed to be the same throughout the universe<\/dd>\r\n<\/dl>\r\n<\/div>","rendered":"<div class=\"textbox learning-objectives\">\n<h3>Learning Objectives<\/h3>\n<p>By the end of this section, you will be able to:<\/p>\n<ul>\n<li>List the significant milestones in the history of gravitation<\/li>\n<li>Calculate the gravitational force between two point masses<\/li>\n<li>Estimate the gravitational force between collections of mass<\/li>\n<\/ul>\n<\/div>\n<p id=\"fs-id1168327959267\">We first review the history of the study of gravitation, with emphasis on those phenomena that for thousands of years have inspired philosophers and scientists to search for an explanation. Then we examine the simplest form of Newton\u2019s law of universal gravitation and how to apply it.<\/p>\n<div id=\"fs-id1168327975150\" class=\"bc-section section\">\n<h3>The History of Gravitation<\/h3>\n<p id=\"fs-id1168325664369\">The earliest philosophers wondered why objects naturally tend to fall toward the ground. Aristotle (384\u2013322 BCE) believed that it was the nature of rocks to seek Earth and the nature of fire to seek the Heavens. Brahmagupta (598~665 CE) postulated that Earth was a sphere and that objects possessed a natural affinity for it, falling toward the center from wherever they were located.<\/p>\n<p>The motions of the Sun, our Moon, and the planets have been studied for thousands of years as well. These motions were described with amazing accuracy by <strong><span class=\"no-emphasis\">Ptolemy<\/span><\/strong> (90\u2013168 CE), whose method of epicycles described the paths of the planets as circles within circles. However, there is little evidence that anyone connected the motion of astronomical bodies with the motion of objects falling to Earth\u2014until the seventeenth century.<\/p>\n<p id=\"fs-id1168328266543\">Nicolaus <strong><span class=\"no-emphasis\">Copernicus<\/span><\/strong> (1473\u20131543) is generally credited as being the first to challenge Ptolemy\u2019s geocentric (Earth-centered) system and suggest a heliocentric system, in which the Sun is at the center of the solar system. This idea was supported by the incredibly precise naked-eye measurements of planetary motions by Tycho <strong><span class=\"no-emphasis\">Brahe<\/span><\/strong> and their analysis by Johannes <strong><span class=\"no-emphasis\">Kepler<\/span><\/strong> and <strong><span class=\"no-emphasis\">Galileo<\/span><\/strong> Galilei. Kepler showed that the motion of each planet is an ellipse (the first of his three laws, discussed in <a class=\"target-chapter\" href=\"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/chapter\/13-5-keplers-laws-of-planetary-motion\/\">Kepler\u2019s Laws of Planetary Motion<\/a>), and Robert Hooke (the same Hooke who formulated Hooke\u2019s law for springs) intuitively suggested that these motions are due to the planets being attracted to the Sun. However, it was Isaac Newton who connected the acceleration of objects near Earth\u2019s surface with the centripetal acceleration of the Moon in its orbit about Earth.<\/p>\n<p id=\"fs-id1168328256234\">Finally, in <a class=\"target-chapter\" href=\"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/chapter\/13-8-einsteins-theory-of-gravity\/\">Einstein\u2019s Theory of Gravity<\/a>, we look at the theory of general relativity proposed by Albert Einstein in 1916. His theory comes from a vastly different perspective, in which gravity is a manifestation of mass warping space and time. The consequences of his theory gave rise to many remarkable predictions, essentially all of which have been confirmed over the many decades following the publication of the theory (including the 2015 measurement of gravitational waves from the merger of two black holes).<\/p>\n<\/div>\n<div id=\"fs-id1168327958865\" class=\"bc-section section\">\n<h3>Newton\u2019s Law of Universal Gravitation<\/h3>\n<p id=\"fs-id1168327941709\"><strong><span class=\"no-emphasis\">Newton<\/span><\/strong> noted that objects at Earth\u2019s surface (hence at a distance of $$ {R}_{\\text{E}} $$ from the center of Earth) have an acceleration of <em>g<\/em>, but the Moon, at a distance of about $$ 60\\,{R}_{\\text{E}}$$, has a centripetal acceleration about $$ {(60)}^{2} $$ times smaller than <em>g<\/em>. He could explain this by postulating that a force exists between any two objects, whose magnitude is given by the product of the two masses divided by the square of the distance between them. We now know that this inverse square law is ubiquitous in nature, a function of geometry for point sources. The strength of any source at a distance <em>r<\/em> is spread over the surface of a sphere centered about the mass. The surface area of that sphere is proportional to $$ {r}^{2}$$. In later chapters, we see this same form in the electromagnetic force.<\/p>\n<div id=\"fs-id1168325679209\">\n<h4>Newton\u2019s Law of Gravitation<\/h4>\n<p id=\"fs-id1168325728231\">Newton\u2019s law of gravitation can be expressed as<\/p>\n<div id=\"fs-id1168327894017\"><a id=\"eq13.1\"><\/a>$${\\overset{\\to }{F}}_{12}=G\\frac{{m}_{1}{m}_{2}}{{r}^{2}}{\\hat{r}}_{12}$$<\/div>\n<p id=\"fs-id1168328260151\">where $$ {\\overset{\\to }{F}}_{12} $$ is the force on object 1 exerted by object 2 and $$ {\\hat{r}}_{12} $$ is a unit vector that points from object 1 toward object 2.<\/p>\n<\/div>\n<p id=\"fs-id1168328167966\">As shown in <a class=\"autogenerated-content\" href=\"#CNX_UPhysics_13_01_NewtonLofG\">(Figure)<\/a>, the $$ {\\overset{\\to }{F}}_{12} $$ vector points from object 1 toward object 2, and hence represents an attractive force between the objects. The equal but opposite force $$ {\\overset{\\to }{F}}_{21} $$ is the force on object 2 exerted by object 1.<\/p>\n<div id=\"CNX_UPhysics_13_01_NewtonLofG\" class=\"wp-caption aligncenter\">\n<div style=\"width: 440px\" class=\"wp-caption aligncenter\"><img loading=\"lazy\" decoding=\"async\" src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195821\/CNX_UPhysics_13_01_NewtonLofG.jpg\" alt=\"The figure shows two circular objects, one smaller, labeled as mass m1 on the lower left, and the larger one labeled m2 on the upper right. The center of each object is labeled C M. A line is drawn joining the center of the objects and is labeled as r. Two red arrows and two black arrows, one each from the center of each object, are drawn toward each other. The black arrow from the center of mass 1 is labeled r hat 1 2 and the red arrow from mass 1 is labeled F 1 2. The black arrow from the center of mass 2 is labeled r hat 2 1 and the red arrow from mass 2 is labeled F 2 1.\" width=\"430\" height=\"343\" \/><\/p>\n<p class=\"wp-caption-text\"><strong>Figure 13.2<\/strong> Gravitational force acts along a line joining the centers of mass of two objects.<\/p>\n<\/div>\n<\/div>\n<p id=\"fs-id1168328271118\">These equal but opposite forces reflect Newton\u2019s third law, which we discussed earlier. Note that strictly speaking, <a class=\"autogenerated-content\" href=\"#fs-id1168327894017\">(Figure)<\/a> applies to point masses\u2014all the mass is located at one point. But it applies equally to any spherically symmetric objects, where <em>r<\/em> is the distance between the centers of mass of those objects. In many cases, it works reasonably well for nonsymmetrical objects, if their separation is large compared to their size, and we take <em>r<\/em> to be the distance between the center of mass of each body.<\/p>\n<\/div>\n<div id=\"fs-id1168328373219\" class=\"bc-section section\">\n<h3>The Cavendish Experiment<\/h3>\n<p id=\"fs-id1168328366420\">A century after Newton published his law of universal gravitation, Henry <strong><span class=\"no-emphasis\">Cavendish<\/span><\/strong> determined the proportionality constant <em>G<\/em> by performing a painstaking experiment. He constructed a device similar to that shown in <a class=\"autogenerated-content\" href=\"#CNX_UPhysics_13_01_Cavendish\">(Figure)<\/a>, in which small masses are suspended from a wire. Once in equilibrium, two fixed, larger masses are placed symmetrically near the smaller ones. The gravitational attraction creates a torsion (twisting) in the supporting wire that can be measured.<\/p>\n<p id=\"fs-id1168325860685\">The constant <em>G<\/em> is called the<strong> universal gravitational constant<\/strong> and Cavendish determined it to be $$ G=6.67\\,\u00d7\\,{10}^{-11}\\,\\text{N}\u00b7{\\text{m}}^{2}{\\text{\/kg}}^{2}$$. The word \u2018universal\u2019 indicates that scientists think that this constant applies to masses of any composition and that it is the same throughout the Universe. The value of <em>G<\/em> is an incredibly small number, showing that the force of gravity is very weak. The attraction between masses as small as our bodies, or even objects the size of skyscrapers, is incredibly small. For example, two 1.0-kg masses located 1.0 meter apart exert a force of $$ 6.7\\,\u00d7\\,{10}^{-11}\\,\\text{N} $$ on each other. This is the weight of a typical grain of pollen.<\/p>\n<div id=\"CNX_UPhysics_13_01_Cavendish\" class=\"wp-caption aligncenter\">\n<div style=\"width: 576px\" class=\"wp-caption aligncenter\"><img loading=\"lazy\" decoding=\"async\" src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195824\/CNX_UPhysics_13_01_Cavendish.jpg\" alt=\"The figure illustrates the Cavendish experiment. A horizontal bar, centered on a stand, supports two spheres of mass M, one at either of its ends. The point where the bar sits on the stand is labeled &quot;pivot&quot;. Just over this bar is a stick holding two spherical objects of mass m, one mass at either of its ends. This bar is suspended from a mirror at the center of the device facing to the right. The mirror is suspended from a fiber. The rotation of the fiber over the axis of the stand is counter-clockwise. A light source on the right side of the device emits a ray of light toward the mirror which is then reflected toward a scale bar which is on the right to the device below the light source.\" width=\"566\" height=\"495\" \/><\/p>\n<p class=\"wp-caption-text\"><strong>Figure 13.3<\/strong> Cavendish used an apparatus similar to this to measure the gravitational attraction between two spheres (m) suspended from a wire and two stationary spheres (M). This is a common experiment performed in undergraduate laboratories, but it is quite challenging. Passing trucks outside the laboratory can create vibrations that overwhelm the gravitational forces.<\/p>\n<\/div>\n<\/div>\n<p id=\"fs-id1168328290504\">Although gravity is the weakest of the four fundamental forces of nature, its attractive nature is what holds us to Earth, causes the planets to orbit the Sun and the Sun to orbit our galaxy, and binds galaxies into clusters, ranging from a few to millions. Gravity is the force that forms the Universe.<\/p>\n<div id=\"fs-id1168328307578\" class=\"problem-solving\">\n<h4>Problem-Solving Strategy: Newton\u2019s Law of Gravitation<\/h4>\n<p id=\"fs-id1168327922730\">To determine the motion caused by the gravitational force, follow these steps:<\/p>\n<ol id=\"fs-id1168328303662\" type=\"1\">\n<li>Identify the two masses, one or both, for which you wish to find the gravitational force.<\/li>\n<li>Draw a free-body diagram, sketching the force acting on each mass and indicating the distance between their centers of mass.<\/li>\n<li>Apply Newton\u2019s second law of motion to each mass to determine how it will move.<\/li>\n<\/ol>\n<\/div>\n<div id=\"fs-id1168328269876\" class=\"textbox examples\">\n<h3>Example<\/h3>\n<h4>A Collision in Orbit<\/h4>\n<p>Consider two nearly spherical <em>Soyuz<\/em> payload vehicles, in orbit about Earth, each with mass 9000 kg and diameter 4.0 m. They are initially at rest relative to each other, 10.0 m from center to center. (As we will see in <a class=\"target-chapter\" href=\"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/chapter\/13-5-keplers-laws-of-planetary-motion\/\">Kepler\u2019s Laws of Planetary Motion<\/a>, both orbit Earth at the same speed and interact nearly the same as if they were isolated in deep space.) Determine the gravitational force between them and their initial acceleration. Estimate how long it takes for them to drift together, and how fast they are moving upon impact.<\/p>\n<h4>Strategy<\/h4>\n<p>We use Newton\u2019s law of gravitation to determine the force between them and then use Newton\u2019s second law to find the acceleration of each. For the <em>estimate<\/em>, we assume this acceleration is constant, and we use the constant-acceleration equations from <a class=\"target-chapter\" href=\"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/chapter\/introduction-3\/\">Motion along a Straight Line<\/a> to find the time and speed of the collision.<\/p>\n<h4>Solution<\/h4>\n<p id=\"fs-id1168325735813\">The magnitude of the force is<\/p>\n<div id=\"fs-id1168056388170\" class=\"unnumbered\">$$|{\\overset{\\to }{F}}_{12}|={F}_{12}=G\\,\\frac{{m}_{1}{m}_{2}}{{r}^{2}}=6.67\\,\u00d7\\,{10}^{-11}\\,\\text{N}\u00b7{\\text{m}}^{2}{\\text{\/kg}}^{2}\\frac{(9000\\,\\text{kg})(9000\\,\\text{kg})}{{(10\\,\\text{m})}^{2}}=5.4\\,\u00d7\\,{10}^{-5}\\text{N.}$$<\/div>\n<p id=\"fs-id1168327940864\">The initial acceleration of each payload is<\/p>\n<div id=\"fs-id1168056081366\" class=\"unnumbered\">$$a=\\frac{F}{m}=\\frac{5.4\\,\u00d7\\,{10}^{-5}\\,\\text{N}}{9000\\,\\text{kg}}=6.0\\,\u00d7\\,{10}^{-9}{\\text{m\/s}}^{2}.$$<\/div>\n<p id=\"fs-id1168328379763\">The vehicles are 4.0 m in diameter, so the vehicles move from 10.0 m to 4.0 m apart, or a distance of 3.0 m each. A similar calculation to that above, for when the vehicles are 4.0 m apart, yields an acceleration of $$ 3.8\\,\u00d7\\,{10}^{-8}\\,{\\text{m\/s}}^{2}$$, and the average of these two values is $$ 2.2\\,\u00d7\\,{10}^{-8}\\,{\\text{m\/s}}^{2}$$. If we assume a constant acceleration of this value and they start from rest, then the vehicles collide with speed given by<\/p>\n<div id=\"fs-id1168056179542\" class=\"unnumbered\">$${v}^{2}={v}_{0}^{2}+2a(x-{x}_{0}),\\,\\text{where}\\,{v}_{0}=0,$$<\/div>\n<p id=\"fs-id1168327886813\">so<\/p>\n<div id=\"fs-id1168056221144\" class=\"unnumbered\">$$v=\\sqrt{2(2.2\\,\u00d7\\,{10}^{-9}\\,\\text{N})(3.0\\,\\text{m})}=3.6\\,\u00d7\\,{10}^{-4}\\,\\,\\text{m\/s.}$$<\/div>\n<p id=\"fs-id1168328173465\">We use $$ {v}^{}={v}_{0}+at $$ to find $$ t=v\\text{\/}a=1.7\\,\u00d7\\,{10}^{4}\\,\\text{s} $$ or about 4.6 hours.<\/p>\n<h4>Significance<\/h4>\n<p>These calculations\u2014including the initial force\u2014are only estimates, as the vehicles are probably not spherically symmetrical. But you can see that the force is incredibly small. Astronauts must tether themselves when doing work outside even the massive International Space Station (ISS), as in <a class=\"autogenerated-content\" href=\"#CNX_UPhysics_13_01_Spacewalk\">(Figure)<\/a>, because the gravitational attraction cannot save them from even the smallest push away from the station.<\/p>\n<div id=\"CNX_UPhysics_13_01_Spacewalk\" class=\"wp-caption aligncenter\">\n<div style=\"width: 498px\" class=\"wp-caption aligncenter\"><img loading=\"lazy\" decoding=\"async\" src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195829\/CNX_UPhysics_13_01_Spacewalk.jpg\" alt=\"A photo of an astronaut on a spacewalk is shown.\" width=\"488\" height=\"489\" \/><\/p>\n<p class=\"wp-caption-text\"><strong>Figure 13.4<\/strong> This photo shows Ed White tethered to the Space Shuttle during a spacewalk. (credit: NASA)<\/p>\n<\/div>\n<\/div>\n<\/div>\n<div id=\"fs-id1168328230996\" class=\"textbox exercises check-understanding\">\n<h3>Check Your Understanding<\/h3>\n<div id=\"fs-id1168327958408\" class=\"problem textbox\">\n<div id=\"fs-id1168328367049\">\n<p id=\"fs-id1168327870892\">What happens to force and acceleration as the vehicles fall together? What will our estimate of the velocity at a collision higher or lower than the speed actually be? And finally, what would happen if the masses were not identical? Would the force on each be the same or different? How about their accelerations?<\/p>\n<\/div>\n<div id=\"fs-id1168327933345\" class=\"solution\">\n<div class=\"qa-wrapper\" style=\"display: block\"><span class=\"show-answer collapsed\" style=\"cursor: pointer\" data-target=\"qfs-id1168327933345\">Show Solution<\/span><\/p>\n<div id=\"qfs-id1168327933345\" class=\"hidden-answer\" style=\"display: none\">\n<p id=\"fs-id1168328312328\">The force of gravity on each object increases with the square of the inverse distance as they fall together, and hence so does the acceleration. For example, if the distance is halved, the force and acceleration are quadrupled. Our average is accurate only for a linearly increasing acceleration, whereas the acceleration actually increases at a greater rate. So our calculated speed is too small. From Newton\u2019s third law (action-reaction forces), the force of gravity between any two objects must be the same. But the accelerations will not be if they have different masses.<\/p>\n<\/div>\n<\/div>\n<\/div>\n<\/div>\n<\/div>\n<p id=\"fs-id1168328270037\">The effect of gravity between two objects with masses on the order of these space vehicles is indeed small. Yet, the effect of gravity on you from Earth is significant enough that a fall into Earth of only a few feet can be dangerous. We examine the force of gravity near Earth\u2019s surface in the next section.<\/p>\n<div id=\"fs-id1168327873949\" class=\"textbox examples\">\n<h3>Example<\/h3>\n<h4>Attraction between Galaxies<\/h4>\n<p>Find the acceleration of our galaxy, the <strong><span class=\"no-emphasis\">Milky Way<\/span><\/strong>, due to the nearest comparably sized galaxy, the <strong><span class=\"no-emphasis\">Andromeda galaxy<\/span><\/strong> (<a class=\"autogenerated-content\" href=\"#CNX_UPhysics_13_01_Androm\">(Figure)<\/a>). The approximate mass of each galaxy is 800 billion solar masses (a solar mass is the mass of our Sun), and they are separated by 2.5 million light-years. (Note that the mass of Andromeda is not so well known but is believed to be slightly larger than our galaxy.) Each galaxy has a diameter of roughly 100,000 light-years $$ (1\\,\\text{light-year}=9.5\\,\u00d7\\,{10}^{15}\\,\\,\\text{m})$$.<\/p>\n<div id=\"CNX_UPhysics_13_01_Androm\" class=\"wp-caption aligncenter\">\n<div style=\"width: 741px\" class=\"wp-caption aligncenter\"><img loading=\"lazy\" decoding=\"async\" src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195834\/CNX_UPhysics_13_01_Androm.jpg\" alt=\"A photograph of the Andromeda galaxy is shown.\" width=\"731\" height=\"491\" \/><\/p>\n<p class=\"wp-caption-text\"><strong>Figure 13.5<\/strong> Galaxies interact gravitationally over immense distances. The Andromeda galaxy is the nearest spiral galaxy to the Milky Way, and they will eventually collide. (credit: Boris \u0160tromar)<\/p>\n<\/div>\n<\/div>\n<h4>Strategy<\/h4>\n<p>As in the preceding example, we use Newton\u2019s law of gravitation to determine the force between them and then use Newton\u2019s second law to find the acceleration of the Milky Way. We can consider the galaxies to be point masses, since their sizes are about 25 times smaller than their separation. The mass of the Sun (see <a class=\"target-chapter\" href=\"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/back-matter\/astronomical-data\/\">Appendix D<\/a>) is $$ 2.0\\,\u00d7\\,{10}^{30}\\,\\text{kg} $$ and a light-year is the distance light travels in one year, $$ 9.5\\,\u00d7\\,{10}^{15}\\,\\text{m}$$.<\/p>\n<h4>Solution<\/h4>\n<p id=\"fs-id1168328323842\">The magnitude of the force is<\/p>\n<div id=\"fs-id1168056208576\" class=\"unnumbered\">$${F}_{12}=G\\,\\frac{{m}_{1}{m}_{2}}{{r}^{2}}=(6.67\\,\u00d7\\,{10}^{-11}\\,\\text{N}\u00b7{\\text{m}}^{2}\\text{\/}{\\text{kg}}^{2})\\frac{{[(800\\,\u00d7\\,{10}^{9})(2.0\\,\u00d7\\,{10}^{30}\\,\\text{kg})]}^{2}}{{[(2.5\\,\u00d7\\,{10}^{6})(9.5\\,\u00d7\\,{10}^{15}\\,\\text{m})]}^{2}}=3.0\\,\u00d7\\,{10}^{29}\\,\\text{N.}$$<\/div>\n<p id=\"fs-id1168327874267\">The acceleration of the Milky Way is<\/p>\n<div id=\"fs-id1168056218734\" class=\"unnumbered\">$$a=\\frac{F}{m}=\\frac{3.0\\,\u00d7\\,{10}^{29}\\,\\text{N}}{(800\\,\u00d7\\,{10}^{9})(2.0\\,\u00d7\\,{10}^{30}\\,\\text{kg})}=1.9\\,\u00d7\\,{10}^{-13}{\\text{m\/s}}^{2}.$$<\/div>\n<h4>Significance<\/h4>\n<p>Does this value of acceleration seem astoundingly small? If they start from rest, then they would accelerate directly toward each other, \u201ccolliding\u201d at their center of mass. Let\u2019s estimate the time for this to happen. The initial acceleration is $$ ~{10}^{-13}\\,{\\text{m\/s}}^{2}$$, so using $$ v=at$$, we see that it would take $$ ~{10}^{13}\\,\\text{s} $$ for each galaxy to reach a speed of 1.0 m\/s, and they would be only $$ ~0.5\\,\u00d7\\,{10}^{13}\\,\\text{m} $$ closer. That is nine orders of magnitude smaller than the initial distance between them. In reality, such motions are rarely simple. These two galaxies, along with about 50 other smaller galaxies, are all gravitationally bound into our local cluster. Our local cluster is gravitationally bound to other clusters in what is called a supercluster. All of this is part of the great cosmic dance that results from gravitation, as shown in <a class=\"autogenerated-content\" href=\"#CNX_UPhysics_13_01_Collide\">(Figure)<\/a>.<\/p>\n<div id=\"CNX_UPhysics_13_01_Collide\" class=\"wp-caption aligncenter\">\n<div style=\"width: 910px\" class=\"wp-caption aligncenter\"><img loading=\"lazy\" decoding=\"async\" src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195841\/CNX_UPhysics_13_01_Collide.jpg\" alt=\"An illustration of the Milky Way galaxy, the Andromeda galaxy (M31), shown above and to the left of the Milky Way, and the Triangulum galaxy (M33) shown above the Andromeda galaxy. The sun is labeled in the Milky way. Arrows pointing from the Milky way toward Andromeda and from Andromeda to the Milky way meet between the two galaxies and are labeled &quot;collision in 4 billion years.&quot;\" width=\"900\" height=\"599\" \/><\/p>\n<p class=\"wp-caption-text\"><strong>Figure 13.6<\/strong> Based on the results of this example, plus what astronomers have observed elsewhere in the Universe, our galaxy will collide with the Andromeda Galaxy in about 4 billion years. (credit: NASA)<\/p>\n<\/div>\n<\/div>\n<\/div>\n<\/div>\n<div id=\"fs-id1168327911320\" class=\"textbox key-takeaways\">\n<h3>Summary<\/h3>\n<ul id=\"fs-id1168328367162\">\n<li>All masses attract one another with a gravitational force proportional to their masses and inversely proportional to the square of the distance between them.<\/li>\n<li>Spherically symmetrical masses can be treated as if all their mass were located at the center.<\/li>\n<li>Nonsymmetrical objects can be treated as if their mass were concentrated at their center of mass, provided their distance from other masses is large compared to their size.<\/li>\n<\/ul>\n<\/div>\n<div id=\"fs-id1168327940992\" class=\"review-conceptual-questions\">\n<h3>Conceptual Questions<\/h3>\n<div id=\"fs-id1168328367169\" class=\"problem textbox\">\n<div id=\"fs-id1168327949431\">\n<p id=\"fs-id1168327949433\">Action at a distance, such as is the case for gravity, was once thought to be illogical and therefore untrue. What is the ultimate determinant of the truth in science, and why was this action at a distance ultimately accepted?<\/p>\n<\/div>\n<div id=\"fs-id1168328304318\" class=\"solution\">\n<div class=\"qa-wrapper\" style=\"display: block\"><span class=\"show-answer collapsed\" style=\"cursor: pointer\" data-target=\"qfs-id1168328304318\">Show Solution<\/span><\/p>\n<div id=\"qfs-id1168328304318\" class=\"hidden-answer\" style=\"display: none\">\n<p id=\"fs-id1168328304320\">The ultimate truth is experimental verification. Field theory was developed to help explain how force is exerted without objects being in contact for both gravity and electromagnetic forces that act at the speed of light. It has only been since the twentieth century that we have been able to measure that the force is not conveyed immediately.<\/p>\n<\/div>\n<\/div>\n<\/div>\n<\/div>\n<div id=\"fs-id1168325860246\" class=\"problem textbox\">\n<div id=\"fs-id1168328371916\">\n<p id=\"fs-id1168328371918\">In the law of universal gravitation, Newton assumed that the force was proportional to the product of the two masses ($$~{m}_{1}{m}_{2}$$). While all scientific conjectures must be experimentally verified, can you provide arguments as to why this must be? (You may wish to consider simple examples in which any other form would lead to contradictory results.)<\/p>\n<\/div>\n<\/div>\n<\/div>\n<div id=\"fs-id1168327952737\" class=\"review-problems textbox exercises\">\n<h3>Problems<\/h3>\n<div id=\"fs-id1168328366602\" class=\"problem textbox\">\n<div id=\"fs-id1168328366604\">\n<p id=\"fs-id1168328238746\">Evaluate the magnitude of gravitational force between two 5-kg spherical steel balls separated by a center-to-center distance of 15 cm.<\/p>\n<\/div>\n<div id=\"fs-id1168325667098\" class=\"solution\">\n<div class=\"qa-wrapper\" style=\"display: block\"><span class=\"show-answer collapsed\" style=\"cursor: pointer\" data-target=\"qfs-id1168325667098\">Show Solution<\/span><\/p>\n<div id=\"qfs-id1168325667098\" class=\"hidden-answer\" style=\"display: none\">\n<p id=\"fs-id1168325667100\">$$7.4\\,\u00d7\\,{10}^{-8}\\,\\text{N}$$<\/p>\n<\/div>\n<\/div>\n<\/div>\n<\/div>\n<div id=\"fs-id1168328379314\" class=\"problem textbox\">\n<div id=\"fs-id1168328379316\">\n<p id=\"fs-id1168328379318\">Estimate the gravitational force between two sumo wrestlers, with masses 220 kg and 240 kg, when they are embraced and their centers are 1.2 m apart.<\/p>\n<\/div>\n<\/div>\n<div id=\"fs-id1168328199977\" class=\"problem textbox\">\n<div id=\"fs-id1168328199979\">\n<p id=\"fs-id1168325664395\">Astrology makes much of the position of the planets at the moment of one\u2019s birth. The only known force a planet exerts on Earth is gravitational. (a) Calculate the gravitational force exerted on a 4.20-kg baby by a 100-kg father 0.200 m away at birth (he is assisting, so he is close to the child). (b) Calculate the force on the baby due to Jupiter if it is at its closest distance to Earth, some $$ 6.29\\,\u00d7\\,{10}^{11}\\,\\text{m} $$ away. How does the force of Jupiter on the baby compare to the force of the father on the baby? Other objects in the room and the hospital building also exert similar gravitational forces. (Of course, there could be an unknown force acting, but scientists first need to be convinced that there is even an effect, much less that an unknown force causes it.)<\/p>\n<\/div>\n<div id=\"fs-id1168328070155\" class=\"solution\">\n<div class=\"qa-wrapper\" style=\"display: block\"><span class=\"show-answer collapsed\" style=\"cursor: pointer\" data-target=\"qfs-id1168328070155\">Show Solution<\/span><\/p>\n<div id=\"qfs-id1168328070155\" class=\"hidden-answer\" style=\"display: none\">\n<p id=\"fs-id1168328070157\">a. $$ 7.01\\,\u00d7\\,{10}^{-7}\\,\\text{N}$$; b. The mass of Jupiter is<\/p>\n<p>$$\\begin{array}{cc} {m}_{\\text{J}}=1.90\\,\u00d7\\,{10}^{27}\\,\\text{kg}\\hfill \\\\ {F}_{\\text{J}}=1.35\\,\u00d7\\,{10}^{-6}\\,\\text{N}\\hfill \\\\ \\frac{{F}_{\\text{f}}}{{F}_{\\text{J}}}=0.521\\hfill \\end{array}$$<\/p><\/div>\n<\/div>\n<\/div>\n<\/div>\n<div id=\"fs-id1168328170296\" class=\"problem textbox\">\n<div id=\"fs-id1168328170298\">\n<p id=\"fs-id1168328170300\">A mountain 10.0 km from a person exerts a gravitational force on him equal to 2.00% of his weight. (a) Calculate the mass of the mountain. (b) Compare the mountain\u2019s mass with that of Earth. (c) What is unreasonable about these results? (d) Which premises are unreasonable or inconsistent? (Note that accurate gravitational measurements can easily detect the effect of nearby mountains and variations in local geology.)<\/p>\n<\/div>\n<\/div>\n<div id=\"fs-id1168327953090\" class=\"problem textbox\">\n<div id=\"fs-id1168328281975\">\n<p id=\"fs-id1168328281977\">The International Space Station has a mass of approximately 370,000 kg. (a) What is the force on a 150-kg suited astronaut if she is 20 m from the center of mass of the station? (b) How accurate do you think your answer would be?<\/p>\n<div id=\"CNX_UPhysics_13_01_ISS_img\" class=\"wp-caption aligncenter\">\n<div style=\"width: 460px\" class=\"wp-caption aligncenter\"><img loading=\"lazy\" decoding=\"async\" src=\"https:\/\/s3-us-west-2.amazonaws.com\/courses-images\/wp-content\/uploads\/sites\/2952\/2018\/01\/31195846\/CNX_UPhysics_13_01_ISS_img.jpg\" alt=\"An image of the international space station is shown.\" width=\"450\" height=\"360\" \/><\/p>\n<p class=\"wp-caption-text\"><strong>Figure 13.33<\/strong> (credit: \u00a9ESA\u2013David Ducros)<\/p>\n<\/div>\n<\/div>\n<\/div>\n<div id=\"fs-id1168328358280\">\n<div class=\"qa-wrapper\" style=\"display: block\"><span class=\"show-answer collapsed\" style=\"cursor: pointer\" data-target=\"q496557\">Show Solution<\/span><\/p>\n<div id=\"q496557\" class=\"hidden-answer\" style=\"display: none\">a. $$ 9.25\\,\u00d7\\,{10}^{-6}\\,\\text{N}$$; b. Not very, as the ISS is not even symmetrical, much less spherically symmetrical.<\/div>\n<\/div>\n<\/div>\n<\/div>\n<div id=\"fs-id1168327933478\" class=\"problem textbox\">\n<div id=\"fs-id1168327885276\">\n<p id=\"fs-id1168327885278\">Asteroid Toutatis passed near Earth in 2006 at four times the distance to our Moon. This was the closest approach we will have until 2060. If it has mass of $$ 5.0\\,\u00d7\\,{10}^{13}\\,\\text{kg}$$, what force did it exert on Earth at its closest approach?<\/p>\n<\/div>\n<\/div>\n<div id=\"fs-id1168328367241\" class=\"problem textbox\">\n<div id=\"fs-id1168327885649\">\n<p id=\"fs-id1168327885651\">(a) What was the acceleration of Earth caused by asteroid Toutatis (see previous problem) at its closest approach? (b) What was the acceleration of Toutatis at this point?<\/p>\n<\/div>\n<div id=\"fs-id1168327911238\" class=\"solution\">\n<div class=\"qa-wrapper\" style=\"display: block\"><span class=\"show-answer collapsed\" style=\"cursor: pointer\" data-target=\"qfs-id1168327911238\">Show Solution<\/span><\/p>\n<div id=\"qfs-id1168327911238\" class=\"hidden-answer\" style=\"display: none\">\n<p id=\"fs-id1168327885653\">a. $$ 1.41\\,\u00d7\\,{10}^{-15}{\\text{m\/s}}^{2}$$; b. $$ 1.69\\,\u00d7\\,{10}^{-4}\\,{\\text{m\/s}}^{2}$$<\/p>\n<\/div>\n<\/div>\n<\/div>\n<\/div>\n<\/div>\n<div class=\"textbox shaded\">\n<h3>Glossary<\/h3>\n<dl id=\"fs-id1168328193986\">\n<dt><strong>Newton\u2019s law of gravitation<\/strong><\/dt>\n<dd id=\"fs-id1168327988168\">every mass attracts every other mass with a force proportional to the product of their masses, inversely proportional to the square of the distance between them, and with direction along the line connecting the center of mass of each<\/dd>\n<\/dl>\n<dl id=\"fs-id1168328252700\">\n<dt><strong>universal gravitational constant<\/strong><\/dt>\n<dd id=\"fs-id1168328252706\">constant representing the strength of the gravitational force, that is believed to be the same throughout the universe<\/dd>\n<\/dl>\n<\/div>\n\n\t\t\t <section class=\"citations-section\" role=\"contentinfo\">\n\t\t\t <h3>Candela Citations<\/h3>\n\t\t\t\t\t <div>\n\t\t\t\t\t\t <div id=\"citation-list-1113\">\n\t\t\t\t\t\t\t <div class=\"licensing\"><div class=\"license-attribution-dropdown-subheading\">CC licensed content, Shared previously<\/div><ul class=\"citation-list\"><li>OpenStax University Physics. <strong>Authored by<\/strong>: OpenStax CNX. <strong>Located at<\/strong>: <a target=\"_blank\" href=\"https:\/\/cnx.org\/contents\/1Q9uMg_a@10.16:Gofkr9Oy@15\">https:\/\/cnx.org\/contents\/1Q9uMg_a@10.16:Gofkr9Oy@15<\/a>. <strong>License<\/strong>: <em><a target=\"_blank\" rel=\"license\" href=\"https:\/\/creativecommons.org\/licenses\/by\/4.0\/\">CC BY: Attribution<\/a><\/em>. <strong>License Terms<\/strong>: Download for free at http:\/\/cnx.org\/contents\/d50f6e32-0fda-46ef-a362-9bd36ca7c97d@10.16<\/li><\/ul><\/div>\n\t\t\t\t\t\t <\/div>\n\t\t\t\t\t <\/div>\n\t\t\t <\/section>","protected":false},"author":311,"menu_order":2,"template":"","meta":{"_candela_citation":"[{\"type\":\"cc\",\"description\":\"OpenStax University Physics\",\"author\":\"OpenStax CNX\",\"organization\":\"\",\"url\":\"https:\/\/cnx.org\/contents\/1Q9uMg_a@10.16:Gofkr9Oy@15\",\"project\":\"\",\"license\":\"cc-by\",\"license_terms\":\"Download for free at http:\/\/cnx.org\/contents\/d50f6e32-0fda-46ef-a362-9bd36ca7c97d@10.16\"}]","CANDELA_OUTCOMES_GUID":"","pb_show_title":"on","pb_short_title":"","pb_subtitle":"","pb_authors":[],"pb_section_license":"all-rights-reserved"},"chapter-type":[],"contributor":[],"license":[56],"class_list":["post-1113","chapter","type-chapter","status-publish","hentry","license-all-rights-reserved"],"part":1099,"_links":{"self":[{"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/pressbooks\/v2\/chapters\/1113","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/pressbooks\/v2\/chapters"}],"about":[{"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/wp\/v2\/types\/chapter"}],"author":[{"embeddable":true,"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/wp\/v2\/users\/311"}],"version-history":[{"count":10,"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/pressbooks\/v2\/chapters\/1113\/revisions"}],"predecessor-version":[{"id":2262,"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/pressbooks\/v2\/chapters\/1113\/revisions\/2262"}],"part":[{"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/pressbooks\/v2\/parts\/1099"}],"metadata":[{"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/pressbooks\/v2\/chapters\/1113\/metadata\/"}],"wp:attachment":[{"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/wp\/v2\/media?parent=1113"}],"wp:term":[{"taxonomy":"chapter-type","embeddable":true,"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/pressbooks\/v2\/chapter-type?post=1113"},{"taxonomy":"contributor","embeddable":true,"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/wp\/v2\/contributor?post=1113"},{"taxonomy":"license","embeddable":true,"href":"https:\/\/courses.lumenlearning.com\/suny-osuniversityphysics\/wp-json\/wp\/v2\/license?post=1113"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}