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'''Differential rotation''' is seen when different parts of a rotating object move with different [[angular velocity|angular velocities]] (rates of [[rotation]]) at different latitudes and/or depths of the body and/or in time. This indicates that the object is not solid. In fluid objects, such as [[accretion disk]]s, this leads to [[Shearing (physics)|shear]]ing. [[galaxy|Galaxies]] and [[protostar]]s usually show differential rotation; examples in the [[Solar System]] include the [[Sun]], [[Jupiter]] and [[Saturn]].
 
== History ==
Around the year 1610, [[Galileo Galilei]] observed [[sunspots]] and calculated the rotation of the [[Sun]]. In 1630, [[Christoph Scheiner]] reported that the Sun had different rotational periods at the poles and at the equator, in good agreement with modern values.
 
== The cause of differential rotation ==
Because of the pre-stellar accretion phase, and the conservation of [[angular momentum]], rotation is induced. Differential rotation is caused by [[convection]] in stars.  This is movement of mass, due to steep temperature gradients from the core outwards. This mass carries a portion of the star’s angular momentum, thus redistributing the angular velocity, possibly even far enough out for the star to lose angular velocity in [[stellar wind]]s. Differential rotation thus depends on temperature differences in adjacent regions.
 
== Measuring differential rotation ==
There are many ways to measure and calculate differential rotation in stars to see if different latitudes have different angular velocities. The most obvious being tracking spots on the stellar surface.
 
By doing [[Helioseismology|helioseismological]] measurements of solar "p-modes" it is possible to deduce the differential rotation. The Sun has very many acoustic modes that oscillate in the interior simultaneously, and the inversion of their frequencies can yield the rotation of the solar interior. This varies with both depth and (especially) latitude.
 
The broadened shapes of absorption lines in the optical spectrum depend on v<sub>rot</sub>sin(i), where ''i'' is the angle between the line of sight and the rotation axis, permitting the study of the rotational velocity’s line-of-sight component v<sub>rot</sub>. This is calculated from [[Fourier transforms]] of the line shapes, using equation (2) below for v<sub>rot</sub> at the equator and poles. See also plot 2.
Solar differential rotation is also seen in magnetograms, images showing the strength and location of solar magnetic fields.
 
== Effects of differential rotation ==
Gradients in angular rotation caused by angular momentum redistribution within the convective layers of a star are expected to be a main driver for generating the large-scale magnetic field, through magneto-hydrodynamical (dynamo) mechanisms in the outer envelopes. The interface between these two regions is where angular rotation gradients are strongest and thus where dynamo processes are expected to be most efficient.
 
The inner differential rotation is one part of the mixing processes in stars, mixing the materials and the heat/energy of the stars.
 
Differential rotation affects stellar optical absorption-[[line spectra]] through [[Doppler broadening|line broadening]] caused by lines being differently [[Doppler-shifted]] across the stellar surface.
 
Solar differential rotation causes shear at the so-called tachocline. This is a region where rotation changes from differential in the convection zone to nearly solid-body rotation in the interior, at 0.71 solar radii from the center.
 
== Calculating differential rotation ==
For observed sunspots, the differential rotation can be calculated as:
:<math>\Omega=\Omega_{0}-\Delta\Omega \sin^{2}\Psi</math>
 
where <math>\Omega_{0}</math> is the rotation rate at the equator, and <math>\Delta\Omega=(\Omega_{0}-\Omega_\mathrm{pole})</math> is the difference in angular velocity between pole and equator, called the strength of the rotational shear. <math>\Psi</math> is the heliographic latitude, measured from the equator.
*The reciprocal of the rotational shear  <math>\frac{2\pi}{\Delta\Omega}</math> is the lap time, i.e. the time it takes for the equator to do a full lap more than the poles.
*The relative differential rotation rate is the ratio of the rotational shear to the equatorial velocity:
:<math>\alpha=\frac{\Delta\Omega}{\Omega_{0}}</math>
 
*The Doppler rotation rate in the Sun (measured from Doppler-shifted absorption lines), can be approximated as:
:<math>\frac{\Omega}{2\pi}(451.5-65.3\cos^{2}\theta - 66.7\cos^{4}\theta)</math>
 
where θ is the co-latitude (measured from the poles).
 
== Differential rotation of the Sun ==
[[File:Tachocline.gif|thumb|right|200px|Internal rotation in the Sun, showing differential rotation in the outer convective region and almost uniform rotation in the central radiative region.]]
{{see also|Solar rotation}}
On the Sun, the study of oscillations revealed that rotation is roughly constant within the whole radiative interior and variable with radius and latitude within the convective envelope. The Sun has an equatorial rotation speed of ~2&nbsp;km/s; its differential rotation implies that the angular velocity decreases with increased latitude. The poles make one rotation every 34.3 days and the equator every 25.05 days, as measured relative to distant stars (sidereal rotation).
 
The highly turbulent nature of solar convection and anisotropies induced by rotation complicate the dynamics of modeling. Molecular dissipation scales on the Sun are at least six orders of magnitude smaller than the depth of the convective envelope. A direct numerical simulation of solar convection would have to resolve this entire range of scales in each of the three dimensions. Consequently, all solar differential rotation models must involve some approximations regarding momentum and heat transport by turbulent motions that are not explicitly computed. Thus, modeling approaches can be classified as either mean-field models or large-eddy simulations according to the approximations.
 
==See also==
* [[Carrington rotation]]
* [[Giovanni Domenico Cassini|Giovanni Cassini]]
* [[Solar nebula]]
* [[Stellar rotation]]
* [[Sunspot]]
 
==Further reading==
* Annu. Rev. Astron. Astrophys. 2003. 41:599-643 {{doi|10.1146/annurev.astro.41.011802.094848}} "''The Internal Rotation of the Sun''"
* David F. Gray, ''Stellar Photospheres; The Observations and Analysis of: Third Edition'', chapter 8, Cambridge University Press, ISBN 978-0-521-85186-2
 
== External links ==
*[http://www.astro.physik.uni-goettingen.de/~areiners/DiffRot/interactive.htm http://www.astro.physik.uni-goettingen.de/~areiners/DiffRot/interactive.htm A simulation of the effects of differential rotation on stellar absorption-line profiles by Ansgar Reiners]
*[http://www.aanda.org/index.php?option=article&access=standard&Itemid=129&url=/articles/aa/full/2002/10/aa1929/aa1929.right.html A. Reiners &  J. H. M. M. Schmitt: On the feasibility of the detection of differential rotation in stellar absorption profiles, Astronomy & Astrophysics 384, 155-162 (2002) - ]
 
*[http://www.es.ucsc.edu/~glatz/sun_giants.html explanation of increased angular velocity at equatorial latitude due to overshoot of mass arriving from heated core]
 
{{DEFAULTSORT:Differential Rotation}}
[[Category:Co-orbital objects]]
[[Category:Astrophysics]]

Latest revision as of 15:45, 12 January 2015

The most vital and required component of your pool maintenance is, cleaning your pool water clean. However, most of you men feel the task as the greatest frustration in preserving a pool.

Its not so! Your pool water needs to spick-and-span. Your swimming pool with clean water will always be an inviting spot for you and notably, itll keep you far from a lot of diseases and infections. Its not a headache rather a simple n enjoyable activity, if you actually enjoy your pool. You just need to keep care of certain things.

You need to be well aware of toxin or pollutants that typically contaminate your swimming pools water. Your swimming pools water generally gets contaminated by toxic wastes, such as dirt, leaves, chemical substance wastes, pollen, spores, germs, and so on. Your sweat, body oils, and physique fluids additionally pollute your swimming pools water. Nonetheless, you could examine these pollutants from getting involved in your swimming pools water and you could even obtain these pollutants from your swimming pool water.

Your pool has a flow pump and filter. Your swimming pool pump makes your pool water move via your swimming pool filter daily, hence it aids to remove undesirable pollutants and disinfected organic products from your swimming pool water.

What you should do is, to inspect that your swimming pool is prepared with a high quality pump and filter. You must additionally keep frequently examining that your pool pump and filter are working well. In case you notice any sort of trouble, you need to obtain it dealt with by an expert.

Sand filters are the most common filter taken in swimming pools nowadays. These filters are considerably easier to preserve compared to the diatomaceous filters. The diatomaceous filters could strain finer bits of gunk, however they call for more upkeep.

Cartridge filters, which are rather basic to maintain, are likewise quite extensively in use these days. Nowadays, zeolite filters are increasing rather popular.

The filters with zeolite, especially the clinoptilolite mineral, could filter bits as finely as diatomaceous filters. Browse here at the link cock rings for sale to check up the reason for this idea. Additionally, the zeolite filters do not need any extra upkeep and they likewise have capacity to absorb ammonia and its complexes, minimizing incorporated chlorine and offensive chlorine smells.

You ought to likewise backwash your swimming pool filter. While filtering system water, some dirt, dirt and various other particles obtain caught in your swimming pool filter, which impair the passage of water through the filter. As outcome, your filter loses performance. Backwashing your filter will send out water in reverse via the filter and clears the trapped dirt out. Itll aid boost the working of your filter.

You need to start your swimming pool pump at the very least 6 - 8 hours every day. There is generally a timer that patterns the pool pump on and off to ensure this constant filtering. Discover extra info on this affiliated article - Browse this URL: ben wa balls video. Your pump will help circulate the pool water and remove floating or put on hold bits of gunk from the water, yet it cant do everything concerning pollutant that have actually worked out to the base of the pool or "stuck" to the wall surfaces; these could just be eliminated by routine brushing and vacuuming of your pool. Therefore, to keep your swimming pool water tidy, you just need to keep checking that your pool pump and filter are working well..

When you loved this informative article and you want to receive more details about health insurance rates (agree with this) i implore you to visit our website.

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