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...Rotating Relativistic Stars. II. Models for Neutron Stars and Supermassive Stars|journal = The Astrophysical Journal|volume = 153|pages = 807|year = 1968|la ...ide [[neutron stars]], [[white dwarfs]] and [[supermassive stars]]. It can be shown that it is an approximation to the [[Kerr metric]] (which describes a ...

Because of the high number of field [[stars]] from the [[Milky_Way#Composition_and_structure|disc of the Milky Way]], i ...BV photometry of 52 stars. They estimated the [[Star cluster|cluster]] to be 910 [[parsec]]s from the [[Sun]], its mean [[Extinction (astronomy)|visual ...

...tar]]'s orbital plane, induced by gravitational perturbations from passing stars. ...aining a large number of stars. Let <math>M_1</math> and <math>M_2</math> be the masses of the two components of the binary whose total mass is <math>M_ ...

...s are necessary. Periodic changes in brightness have long been observed in stars which indicate cooler or brighter [[starspot]]s on the surface. These spots ...t used to map chemical peculiarities on the surface of [[Ap and Bp star|Ap stars]]. For mapping starspots it was first used by [[Steven Vogt]] and Donald Pe ...

...ts temperature is over 10,000 K,<ref name=manick/> and it is hot enough to be classified as a B-type [[blue giant]], as well as being the hottest [[RV Ta However, the star may be less luminous than it seems, as its spectral energy distribution is contami ...

...s|the most massive]] and [[List of most luminous stars|most luminous known stars]].<ref name=wu/> ...pectral type of O2-3.5If^*. The star is one of the most luminous stars known, with a luminosity of {{solar luminosity|4,365,000}}, and has a tempe ...

...iv = astro-ph/0301257 }}</ref> is the radius at which the enclosed mass in stars equals twice ''M''_BH, i.e. ...inition compares the force from the black hole to the local force from the stars. ...

...making V Coronae Borealis [[List of largest known stars|one of the largest stars]] so far discovered.<ref name=Danilovich2015/> If placed in the center of t ...title=New observations and models of circumstellar CO line emission of AGB stars in the Herschel SUCCESS programme |bibcode=2015A&A...581A..60D |journal=Ast ...

...m from gases, the cosmic winds that push the gases away are preventing new stars from forming and are ultimately playing a role in galaxy evolution.<ref nam ...bination of these hot and cooling flows that cause cosmic wind. In smaller stars, such as the Sun, the wind comes from the Sun's [[Stellar corona|corona]] a ...

...e at ESO’s [[La Silla Observatory]] in Chile.<ref>{{cite web|title=Sibling Stars|url=http://www.eso.org/public/news/eso1534/|access-date=19 August 2015}}</r ...drogen]] and [[helium]].<ref name=aaa424/> The combined mass of the active stars in this cluster is about 630 times the [[mass of the Sun]].<ref name=aaa386 ...

...l |bibcode=2018MNRAS.480.3706K |title=On the evolutionary state of massive stars in transition phases in M33 |last1=Kourniotis |first1=M. |last2=Kraus |firs ...ctrum based on some assumptions about the relative sizes of the two [[Star|stars]] suggests a secondary around half a million times as luminous as the [[Sun ...

...] of its component [[star]]s. The distance to the stellar system must also be known. ...e virial theorem. However, it requires that two components of the velocity be known for every star, rather than just one for the virial theorem.<ref>{{Ci ...

{{Short description|Method to determine the temperature of central stars of planetary nebulae}} The '''Zanstra method''' is a method to determine the temperature of central stars of [[planetary nebulae]]. It was developed by [[Herman Zanstra]] in 1927. ...

...ournal|title=Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system|author=Gontcharov, G. A.|date=2006|journal=Astronomy Let ...agnitude]] is 6.80,<ref name=Ducati/> making it not quite bright enough to be seen with the [[naked eye]]. ...

...=The wind speeds, dust content, and mass-loss rates of evolved AGB and RSG stars at varying metallicity|year=2016|journal=[[Monthly Notices of the Royal Ast ...rger than of the Sun, making it one of the [[List of largest stars|largest stars]] discovered so far. If placed at the center of the [[Solar System]], its [ ...

...oved sections have been commented out instead of deleted, in case they can be improved and put back into the article.--> ...or the [[Magnetohydrodynamics#Ideal MHD equations|ideal MHD equations]] to be a good approximation, but this is not true in star forming regions where th ...

...ry/optical-IR-prod/wds/orb6|title=Sixth Catalog of Orbits of Visual Binary Stars|work=United States Naval Observatory|access-date=2017-03-11|archive-date=20 ...]. Its apparent magnitude is 3.30,<ref name="Ducati"/> meaning that it can be seen with the naked eye ''(see [[Bortle scale]])''. ...

...n the sky to calibrate the detector, so for general purposes, any star may be used in the sky that has a known apparent magnitude.<ref name=":1">{{Cite w ...[[bolometric magnitude]] and apparent bolometric magnitude zero points to be 3.0128×10²⁸ W and 2.51802×10⁻⁸ W/m², respe ...

...ts significantly different from the stellar disk. This includes metal-poor stars (with low [Fe/H] < -1), which likely belong to the [[stellar halo]] or [[Ac ...first=George|date=1962|title=Abundances in G Dwarfs. VI. A Survey of Field Stars |journal=The Astrophysical Journal Supplement Series|language=en|volume=6|p ...

...thor1=Stahler, Steven |author2=Palla, Francesco | title = The Formation of Stars | publisher = [[Wiley-VCH]] | isbn = 3-527-40559-3 | year = 2004 | url = ht ...tinuum as the true one."<ref name="formation_of_stars"/> This equation can be applied to either [[emission (electromagnetic radiation)|emission]] or [[ab ...