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Stellar-dynamical models of systems such as galaxies or star clusters are often compared with or tested against stellar-kinematic data to study their evolutionary history and mass distributions, and to detect the presence of dark matter or supermassive black holes through their gravitational influence on stellar orbits.
The component of stellar motion toward or away from the Sun, known as radial velocity , can be measured from the spectrum shift caused by the Doppler effect.
The transverse, or proper motion must be found by taking a series of positional determinations against more distant objects.
Once the distance to a star is determined through astrometric means such as parallax , the space velocity can be computed. The latter is typically taken as a position at the Sun's present location that is following a circular orbit around the Galactic Center at the mean velocity of those nearby stars with low velocity dispersion.
Stellar kinematics yields important astrophysical information about stars, and the galaxies in which they reside. Stellar kinematics data combined with astrophysical modeling produces important information about the galactic system as a whole.
Measured stellar velocities in the innermost regions of galaxies including the Milky Way have provided evidence that many galaxies host supermassive black holes at their center.
In farther out regions of galaxies such as within the galactic halo, velocity measurements of globular clusters orbiting in these halo regions of galaxies provides evidence for dark matter.
Both of these cases derive from the key fact that stellar kinematics can be related to the overall potential in which the stars are bound.
This means that if accurate stellar kinematics measurements are made for a star or group of stars orbiting in a certain region of a galaxy, the gravitational potential and mass distribution can be inferred given that the gravitational potential in which the star is bound produces its orbit and serves as the impetus for its stellar motion.
Examples of using kinematics combined with modeling to construct an astrophysical system include:.
In the Gaia data release 2 has yielded an unprecedented number of high quality stellar kinematic measurements as well as stellar parallax measurements which will greatly increase our understanding of the structure of the Milky Way.
The Gaia data has also made it possible to determine the proper motions of many objects whose proper motions were previously unknown, including the absolute proper motions of 75 globular clusters orbiting at distances as far as 21 kpc.
Stars within galaxies may be classified based on their kinematics. For example, the stars in the Milky Way can be subdivided into two general populations, based on their metallicity , or proportion of elements with atomic numbers higher than helium.
Among nearby stars, it has been found that population I stars with higher metallicity are generally located in the stellar disk while older population II stars are in random orbits with little net rotation.
These are most likely groups of stars that share a common point of origin in giant molecular clouds. There are many additional ways to classify stars based on their measured velocity components, and this provides detailed information about the nature of the star's formation time, its present location, and the general structure of the galaxy.
As a star moves in a galaxy, the smoothed out gravitational potential of all the other stars and other mass within the galaxy plays a dominant role in determining the stellar motion.
Measurements of an individual star's kinematics can identify stars that are peculiar outliers such as a high-velocity star moving much faster than its nearby neighbors.
The velocity is also sometimes defined as supersonic relative to the surrounding interstellar medium. The three types of high-velocity stars are: runaway stars, halo stars and hypervelocity stars.
High-velocity stars were studied by Jan Oort, who used their kinematic data to predict that high-velocity stars have very little tangential velocity.
A runaway star is one that is moving through space with an abnormally high velocity relative to the surrounding interstellar medium.
The proper motion of a runaway star often points exactly away from a stellar association , of which the star was formerly a member, before it was hurled out.
Multiple mechanisms may accelerate the same runaway star. For example, a massive star that was originally ejected due to gravitational interactions with its stellar neighbors may itself go supernova , producing a remnant with a velocity modulated by the supernova kick.
If this supernova occurs in the very nearby vicinity of other stars, it is possible that it may produce more runaways in the process.
Tracing their motions back, their paths intersect near to the Orion Nebula about 2 million years ago. Barnard's Loop is believed to be the remnant of the supernova that launched the other stars.
Another example is the X-ray object Vela X-1 , where photodigital techniques reveal the presence of a typical supersonic bow shock hyperbola.
Halo stars are very old stars that do not share the motion of the Sun or most other stars in the solar neighbourhood which are in similar circular orbits around the center of the Milky Way, within its disk.
Instead, the halo stars travel in elliptical orbits, often inclined to the disk, which take them well above and below the plane of the Milky Way.
I'd tuk one ob de guns—you warn't in de hous, massa, so I cudn't ax you. Some boy sho' must ob busted his head open, to need tyin' up so bad.
Nihil ob id apud Helvetios agendum de lis rebus qu Christi gloriam possunt augere. Gulf of, an inlet of the Arctic Ocean. Nicole Napier, M.
Jennifer Shark, C. Cecilia Warpinski Stuopis, M. Chana S. Wasserman, M. Chief of Obstetrics and Gynecology. Jennifer Williams, C. In extension to the compress function posted below, here's a nifty little class that improves the idea a bit.
Basically, running that compress function for all your CSS for every single page load is clearly far less than optimal, especially since the styles will change only infrequently at the very worst.
The contents of each file are saved in compress 'd form in a cache file that is only recreated when the corresponding source CSS changes.
To fix, remove the flush. Spent several hours discovering this. Apache 1. If you're using Apache 1. I assume you all know how to build compression classes and use them in your programs, but none has yet to offer the speed and robustness of a binary-compiled module.
Furthermore, such modules also log the "compressable" hit in the web log file, thus allowing your favorite web anaysing program to show you reports of bandwidth saved.
Having said that, you might consider the following two modules for Apache: 1 Apache 1. I think it's worth noting that while you can't call any output functions such as echo or print from within a callback function, you can still send headers presumably including cookies, haven't checked.
This can be handy if you want to avoid replacing header values that are uncertain. For example if your code may return an image, but you don't want to set content type until you're sure that the image can be sent successfully, you can use the callback to leave the decision right until the very last moment, by which point you're hopefully sure of what's being sent in the HTTP body.
When a fatal error is thrown, PHP will output the current buffer of Output-Control without postprocessing before printing the error message.
If you are working with several output control levels, this might not result in the desired behavior. You can use an output callback handler to handle this and discard the output.
Hysterectomy B-Lynch suture. Authority control NDL : Categories : Obstetrics Gynaecology. Hidden categories: Articles with limited geographic scope from August Pages in non-existent country centric categories Wikipedia articles with NDL identifiers.
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