|
|
| (One intermediate revision by the same user not shown) |
| Line 1: |
Line 1: |
| [[File:Shoemaker-levy-tidal-forces.jpg|thumbnail|300px|Figure 1: [[Comet Shoemaker-Levy 9]] in 1994 after breaking up under the influence of [[Jupiter]]'s tidal forces during a previous pass in 1992.]]
| | The writer is called Irwin Wunder but it's not the most masucline name out there. For years I've been working as a payroll clerk. The preferred pastime for my kids and me is to play baseball but I haven't made a dime with it. Years ago he moved to North Dakota and his family members enjoys it.<br><br>Here is my web blog: [https://clouditcanada.zendesk.com/entries/97443026-Yeast-Infection-Tips-You-Have-To-Remember zendesk.com] |
| | |
| The '''tidal force''' is a secondary effect of the [[force]] of [[gravity]] and is responsible for the [[tide]]s. It arises because the gravitational force exerted by one body on another is not constant across its [[diameter]]. The nearest side is attracted more strongly than the farthest side. Thus, the tidal force is differential. Consider the gravitational attraction of the moon on the oceans nearest the moon, the solid earth and the oceans farthest from the moon. There is a mutual attraction between the moon and the solid earth which can be considered to act on its centre of mass. However, the near oceans are more strongly attracted and, since they are fluid, they approach the moon slightly, causing a high tide. The far oceans are attracted less. The attraction on the far-side oceans could be expected to cause a low tide but since the solid earth is attracted ( accelerated ) more strongly towards the moon, there is a ''relative'' acceleration of those waters in the outwards direction. Viewing the Earth as a whole, we see that all its mass experiences a mutual attraction with that of the moon but the near oceans more so than the far oceans, leading to a separation of the two. | |
| | |
| In a more general usage in [[celestial mechanics]], the expression 'tidal force' can refer to a situation in which a body or material (for example, tidal water, or the Moon) is mainly under the gravitational influence of a second body (for example, the Earth), but is also perturbed by the gravitational effects of a third body (for example, by the Moon in the case of tidal water, or by the Sun in the case of the Moon). The perturbing force is sometimes in such cases called a tidal force<ref>[http://adsabs.harvard.edu/full/1977SvAL....3...96A "On the tidal force"], I N Avsiuk, in "Soviet Astronomy Letters", vol.3 (1977), pp. 96–99</ref> (for example, the [[Lunar theory#Newton|perturbing force on the Moon]]): it is the difference between the force exerted by the third body on the second and the force exerted by the third body on the first.<ref>See p.509 in [http://books.google.com/books?id=2QVmiMW0O0MC&pg=PA509&lpg=PA509&dq=%22tidal+force%22+perturb&source=bl&ots=46yDoQd9k7&sig=bep2Wi1UfMQhsfmHAd1N2VfWTso&hl=en&ei=J1GYSvTeDIKNjAe8lvm_BQ&sa=X&oi=book_result&ct=result&resnum=10#v=onepage&q=%22tidal%20force%22%20perturb&f=false "Astronomy: a physical perspective"], M L Kutner (2003).</ref>
| |
| | |
| == Explanation ==
| |
| | |
| [[File:Field tidal.png|thumb|left|260px|Figure 2: The Moon's gravity differential field at the surface of the Earth is known (along with another and weaker differential effect due to the Sun) as the Tide Generating Force. This is the primary mechanism driving tidal action, explaining two tidal equipotential bulges, and accounting for two high tides per day. In this figure, the Moon is either on the right side or on the left side of the Earth (at center). The '''outward''' direction of the arrows on the right and left indicates that where the Moon is overhead (or at the [[nadir]]) its perturbing force opposes that between the earth and ocean. The '''inward''' direction of the arrows at top and bottom indicates that where the Moon is 90 degrees away from overhead. Its effect is perpendicual and does not change the strength of the Earth's attraction on the ocean.]]
| |
| | |
| When a body (body 1) is acted on by the gravity of another body (body 2), the field can vary significantly on body 1 between the side of the body facing body 2 and the side facing away from body 2. Figure 2 shows the differential force of gravity on a spherical body (body 1) exerted by another body (body 2). These so-called ''tidal forces'' cause strains on both bodies and may distort them or even, in extreme cases, break one or the other apart.<ref name=Penrose>{{cite book |title=The Emperor's New Mind: Concerning Computers, Minds, and the Laws of Physics |author=R Penrose |page=264 |url=http://books.google.com/books?id=oI0grArWHUMC&pg=PA264&vq=tidal&dq=tidal+force
| |
| | isbn=0-19-286198-0 |year=1999 |publisher=Oxford University Press}}</ref> The [[Roche limit]] is the distance from a planet at which tidal effects would cause an object to disintegrate because the differential force of gravity from the planet overcomes the attraction of the parts of the object for one another.<ref name=Blanc>{{cite book |title=The Solar System |page=16 |url=http://books.google.com/books?id=Je61Y7UbqWgC&pg=PA16&vq=tide&dq=tidal+force#PPA16,M1
| |
| | author=Thérèse Encrenaz, J -P Bibring, M Blanc |isbn=3-540-00241-3 |year=2003 |publisher=Springer }}</ref> These strains would not occur if the gravitational field were uniform, because a uniform [[field (physics)|field]] only causes the entire body to accelerate together in the same direction and at the same rate.
| |
| | |
| == Effects of tidal forces ==
| |
| | |
| [[File:Saturn-cassini-March-27-2004.jpg|thumbnail|300px|Figure 3: [[Saturn]]'s rings are inside the orbits of its principal moons. Tidal forces oppose gravitational coalescence of the material in the rings to form moons.<ref name=MacKay>{{cite book |author=R. S. MacKay, J. D. Meiss |title=Hamiltonian Dynamical Systems: A Reprint Selection |page=36 |url=http://books.google.com/books?id=uTeqNsyj86QC&pg=PA36&dq=tidal+force |isbn=0-85274-205-3 |year=1987 |publisher=CRC Press}}</ref>]]
| |
| In the case of an infinitesimally small elastic sphere, the effect of a tidal force is to distort the shape of the body without any change in volume. The sphere becomes an [[ellipsoid]] with two bulges, pointing towards and away from the other body. Larger objects distort into an [[ovoid]], and are slightly compressed, which is what happens to the Earth's oceans under the action of the Moon. The Earth and Moon rotate about their common center of mass or [[barycenter]], and their gravitational attraction provides the [[centripetal force]] necessary to maintain this motion. To an observer on the Earth, very close to this barycenter, the situation is one of the Earth as body 1 acted upon by the gravity of the Moon as body 2. All parts of the Earth are subject to the Moon's gravitational forces, causing the water in the oceans to redistribute, forming bulges on the sides near the Moon and far from the Moon.<ref name=Americana>{{cite book |title=The Encyclopedia Americana: A Library of Universal Knowledge |author=Rollin A Harris |pages=611–617 |url=http://books.google.com/books?id=r8BPAAAAMAAJ&pg=PA612&dq=tidal+force#PPA612,M1
| |
| | publisher=Encyclopedia Americana Corp. |year=1920 |edition=Vol. 26 }}</ref>
| |
| | |
| When a body rotates while subject to tidal forces, internal friction results in the gradual dissipation of its rotational kinetic energy as heat. If the body is close enough to its primary, this can result in a rotation which is tidally locked to the orbital motion, as in the case of the Earth's moon. Tidal heating produces dramatic volcanic effects on Jupiter's moon [[Io (moon)|Io]]. Stresses caused by tidal forces also cause a regular monthly pattern of [[moonquake]]s on Earth's Moon.
| |
| | |
| Tidal forces contribute to ocean currents, which moderate global temperatures by transporting heat energy toward the poles. It has been suggested that in addition to other factors, [[beat (acoustics)|harmonic beat]] variations in tidal forcing may contribute to climate changes.<ref>{{cite web
| |
| | title =Millennial Climate Variability: Is There a Tidal Connection?
| |
| | url =http://dx.doi.org/10.1175/1520-0442(2002)015{{urlencode:<0370:MCVITA>2.0.CO;2|PATH}}
| |
| }}</ref>
| |
| | |
| Tidal effects become particularly pronounced near small bodies of high mass, such as [[neutron star]]s or [[black hole]]s, where they are responsible for the "[[spaghettification]]" of infalling matter. Tidal forces create the oceanic [[tide]] of [[Earth]]'s oceans, where the attracting bodies are the [[Moon]] and, to a lesser extent, the [[Sun]].
| |
| | |
| Tidal forces are also responsible for [[tidal locking]] and [[tidal acceleration]].
| |
| | |
| == Categories of gravitational forces ==
| |
| [[File:Inseparable galactic twins.jpg|thumb|Tidal force is responsible for the merge of galactic pair [[MRK 1034]].<ref>{{cite news|title=Inseparable galactic twins|url=http://www.spacetelescope.org/images/potw1325a/|accessdate=12 July 2013|newspaper=ESA/Hubble Picture of the Week}}</ref> ]]
| |
| | |
| There are four different ways to categorize the gravitational forces acting on the earth while it rotates around the sun. The first category is there are the tides resulting from the combined pull of the Moon and the Sun. The pull of the Moon and the Sun affects the movement of the atmosphere and oceans, as well as stress in the Earth's crust. Second category considers the changing positions of other planets in relation to the Earth. The third category of gravitational forces that affect tidal forces involves planetary motions affecting the Sun's circulation and solar activity. Fourth and final category considers orbital affects of those motions. Changes in the speed of the Earth's orbit may affect small movements of the Sun, so basically small periodic influences on the Earth's climate and tidal forces.<ref>{{cite book|last=Burroughs|first=William James|title=Climate change: a multidisciplinary approach|year=2007|publisher=Cambridge University Press|location=Cambridge|isbn=9780521870153|edition=2nd}}</ref>
| |
| | |
| == Mathematical treatment ==
| |
| | |
| For a given (externally-generated) gravitational field, the '''tidal acceleration''' at a point with respect to a body is obtained by [[Euclidean vector#Addition and subtraction|vectorially subtracting]] the gravitational acceleration at the center of the body (due to the given externally-generated field) from the gravitational acceleration (due to the same field) at the given point. Correspondingly, the term '''''tidal force''''' is used to describe the forces due to tidal acceleration. Note that for these purposes the only gravitational field considered is the external one; the gravitational field of the body (as shown in the graphic) is not relevant. (In other words the comparison is with the conditions at the given point as they would be if there were no externally-generated field acting unequally at the given point and at the center of the reference body. The externally-generated field is usually that produced by a perturbing third body, often the Sun or the Moon in the frequent example-cases of points on or above the Earth's surface in a geocentric reference frame.) | |
| | |
| [[File:Tidal-forces.svg|thumb|right|Figure 4: Graphic of tidal forces. The top picture shows the gravity field of a body to the right, the lower shows their residual once the field at the centre of the sphere is subtracted; this is the tidal force. See Figure 2 for a more detailed version]]
| |
| Tidal acceleration does not require rotation or orbiting bodies; for example, the body may be [[freefall]]ing in a straight line under the influence of a gravitational field while still being influenced by (changing) tidal acceleration.
| |
| | |
| By [[Newton's law of universal gravitation]] and laws of motion, a body of mass ''m'' a distance ''R'' from the center of a sphere of mass ''M'' feels a force <math>\vec F_g</math> equivalent to an acceleration <math>\vec a_g</math>, where:
| |
| | |
| : <math>\vec F_g = - \hat r ~ G ~ \frac{M m}{R^2}</math> . . . , and. . . <math>\vec a_g = - \hat r ~ G ~ \frac{M}{R^2}</math> . . . ,
| |
| | |
| where <math>\hat r</math> is a [[unit vector]] pointing from the body ''M'' to the body ''m'' (here, acceleration from ''m'' towards ''M'' has negative sign).
| |
| | |
| Consider now the acceleration due to the sphere of mass ''M'' experienced by a particle in the vicinity of the body of mass ''m''. With ''R'' as the distance from the center of ''M'' to the center of ''m'', let ∆''r'' be the (relatively small) distance of the particle from the center of the body of mass ''m''. For simplicity, distances are first considered only in the direction pointing towards or away from the sphere of mass ''M''. If the body of mass ''m'' is itself a sphere of radius ∆''r'', then the new particle considered may be located on its surface, at a distance (''R'' ± ''∆r'') from the centre of the sphere of mass ''M'', and ''∆r'' may be taken as positive where the particle's distance from ''M'' is greater than ''R''. Leaving aside whatever gravitational acceleration may be experienced by the particle towards ''m'' on account of ''m'''s own mass, we have the acceleration on the particle due to gravitational force towards ''M'' as:
| |
| | |
| : <math>\vec a_g = - \hat r ~ G ~ \frac{M}{(R \pm \Delta r)^2}</math>
| |
| | |
| Pulling out the ''R''<sup>2</sup> term from the denominator gives:
| |
| | |
| : <math>\vec a_g = - \hat r ~ G ~ \frac{M}{R^2} ~ \frac{1}{(1 \pm \Delta r / R)^2}</math>
| |
| | |
| The [[Maclaurin series]] of 1/(1 + ''x'')<sup>2</sup> is 1 – 2''x'' + 3''x''<sup>2</sup> – ..., which gives a series expansion of:
| |
| | |
| : <math>\vec a_g = - \hat r ~ G ~ \frac{M}{R^2} \pm \hat r ~ G ~ \frac{2 M }{R^2} ~ \frac{\Delta r}{R} - \cdots </math>
| |
| | |
| The first term is the gravitational acceleration due to ''M'' at the center of the reference body <math>m</math>, i.e., at the point where <math>\Delta r</math> is zero. This term does not affect the observed acceleration of particles on the surface of ''m'' because with respect to ''M'', ''m'' (and everything on its surface) is in free fall. When the force on the far particle is subtracted from the force on the near particle, this first term cancels, as do all other even-order terms. The remaining (residual) terms represent the difference mentioned above and are tidal force (acceleration) terms. When ∆''r'' is small compared to ''R'', the terms after the first residual term are very small and can be neglected, giving the approximate tidal acceleration <math>\vec a_t</math>(axial) for the distances ∆''r'' considered, along the axis joining the centers of ''m'' and ''M'':
| |
| | |
| : <math>\vec a_t</math>(axial) <math> ~ \approx ~ \pm ~ \hat r ~ 2 \Delta r ~ G ~ \frac{M}{R^3} </math>
| |
| | |
| When calculated in this way for the case where ∆''r'' is a distance along the axis joining the centers of ''m'' and ''M'', <math>\vec a_t</math> is directed outwards from to the center of ''m'' (where ∆''r'' is zero).
| |
| | |
| Tidal accelerations can also be calculated away from the axis connecting the bodies ''m'' and ''M'', requiring a [[Euclidean vector|vector]] calculation. In the plane perpendicular to that axis, the tidal acceleration is directed inwards (towards the center where ∆''r'' is zero), and its magnitude is <math> | \vec a_t</math>(axial)<math> | /2 </math> in linear approximation as in Figure 2.
| |
| | |
| The tidal accelerations at the surfaces of planets in the Solar System are generally very small. For example, the lunar tidal acceleration at the Earth's surface along the Moon-Earth axis is about 1.1 × 10<sup>−7</sup> g, while the solar tidal acceleration at the Earth's surface along the Sun-Earth axis is about 0.52 × 10<sup>−7</sup> g, where g is the [[standard gravity|gravitational acceleration]] at the Earth's surface. Hence the tide-raising force (acceleration) due to the Sun is about 45% of that due to the Moon.<ref>{{cite book
| |
| | title=Admiralty manual of navigation, Volume 1
| |
| | last1=The Admiralty
| |
| | publisher=The Stationery Office
| |
| | year=1987
| |
| | isbn=0-11-772880-2
| |
| | page=277
| |
| | url=http://books.google.com/books?id=GCgXCxG4VLcC}}, [http://books.google.com/books?id=GCgXCxG4VLcC&pg=PA277 Chapter 11, p. 277]
| |
| </ref> The solar tidal acceleration at the Earth's surface was first given by Newton in the '[[Philosophiæ Naturalis Principia Mathematica|Principia]]'.<ref>{{cite book
| |
| | title=The mathematical principles of natural philosophy, Volume 2
| |
| | first1=Isaac
| |
| | last1=Newton
| |
| | year=1729
| |
| | isbn=0-11-772880-2
| |
| | page=307
| |
| | url=http://books.google.com/books?id=6EqxPav3vIsC}}, [http://books.google.com/books?id=6EqxPav3vIsC&pg=PA307 Book 3, Proposition 36, Page 307] Newton put the force to depress the sea at places 90 degrees distant from the Sun at "1 to 38604600" (in terms of ''g''), and wrote that the force to raise the sea along the Sun-Earth axis is "twice as great", i.e. 2 to 38604600, which comes to about 0.52 × 10<sup>-7</sup> ''g'' as expressed in the text.</ref>
| |
| | |
| == See also ==
| |
| | |
| * [[Amphidrome]]
| |
| * [[Tidal resonance]]
| |
| * [[Galactic tide]]
| |
| | |
| == References ==
| |
| {{reflist}}
| |
| | |
| == External links ==
| |
| * [http://burro.astr.cwru.edu/Academics/Astr221/Gravity/tides.html Gravitational Tides] by J. Christopher Mihos of [[Case Western Reserve University]]
| |
| * [http://www.astronomycast.com/solar-system/episode-47-tidal-forces/ Audio: Cain/Gay – Astronomy Cast] Tidal Forces – July 2007.
| |
| * {{cite web|last=Gray|first=Meghan|title=Tidal Forces|url=http://www.sixtysymbols.com/videos/tides.htm|work=Sixty Symbols|publisher=[[Brady Haran]] for the [[University of Nottingham]]|coauthors=Merrifield, Michael}}
| |
| *{{cite web| url=http://members.aei.mpg.de/amaro-seoane/stellar-collisions/stellar-collisions-tidal-disruption-of-a-star-by-a-massive-black-hole/| title=Pau Amaro Seoane MODEST working group 4 "Tidal disruption of a star by a massive black hole"| accessdate=2013-05-30}}
| |
| {{physical oceanography}}
| |
| | |
| [[Category:Gravitation]]
| |
| [[Category:Force]]
| |
| [[Category:Tides]]
| |
| [[Category:Effects of gravitation]]
| |