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- ...[Albireo]], a well-known coloured double star. Compare the colour of other stars in [http://antwrp.gsfc.nasa.gov/apod/ap050830.html] ]] '''''On the coloured light of the binary stars and some other stars of the heavens''''' or in the original German '''{{lang|de|Über das farbige ...19 KB (3,075 words) - 08:14, 3 December 2024
- ...]] and [[brown dwarfs]] which are the least voluminous known (the smallest stars by volume). ===Notable small stars=== ...149 KB (20,469 words) - 03:47, 17 February 2025
- ...cts are also known under the names '''XDINS''' (X-ray Dim Isolated Neutron Stars) or simply '''XINS'''.<ref name="Potekhin15">{{harvnb|Potekhin|De Luca|Pons ...red parsecs), middle-age (several hundred thousand years) isolated neutron stars emitting soft X-rays due to cooling. The cooling is confirmed by the [[blac ...16 KB (2,181 words) - 18:43, 26 December 2024
- ...assiopeiae Sol VY Canis Majoris - 2019-05-14.svg|320px|center|Some massive stars compared to our Sun ( one single grey pixel in the 'Full resolution' image ...4 KB (600 words) - 03:25, 23 August 2023
- Below there are lists the nearest stars separated by [[spectral type]]. The scope of the list is still restricted t == List of nearest M-type stars == ...189 KB (24,909 words) - 01:10, 30 January 2025
Page text matches
- ...Rotating Relativistic Stars. II. Models for Neutron Stars and Supermassive Stars|journal = The Astrophysical Journal|volume = 153|pages = 807|year = 1968|la ...e spacetime outside [[neutron stars]], [[white dwarfs]] and [[supermassive stars]]. It can be shown that it is an approximation to the [[Kerr metric]] (whic ...3 KB (386 words) - 19:59, 30 May 2024
- * <math>F_{HZ}</math>, the fraction of stars with rocky planets in the habitable zone, in Seager's variant of the Drake ...384 bytes (56 words) - 18:11, 25 August 2023
- Because of the high number of field [[stars]] from the [[Milky_Way#Composition_and_structure|disc of the Milky Way]], i ...photometry]] for 171 of its stars and photoelectric UBV photometry of 52 stars. They estimated the [[Star cluster|cluster]] to be 910 [[parsec]]s from th ...4 KB (474 words) - 04:53, 5 April 2021
- ...tar]]'s orbital plane, induced by gravitational perturbations from passing stars. ...and that is embedded in a [[stellar system]] containing a large number of stars. Let <math>M_1</math> and <math>M_2</math> be the masses of the two compon ...6 KB (1,003 words) - 17:27, 9 November 2019
- ...rac{1}{4}+\frac{1}{4}\sqrt{1+4\phi}\approx 0.933\,380\,199\,59</math>, the stars have five equal angles of <math>\arccos(\xi)\approx 21.031\,988\,967\,51^{\ ...2 KB (219 words) - 23:30, 27 December 2022
- ...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 ...7 KB (1,065 words) - 23:30, 16 November 2024
- ...g|first5=Katrien|date=2018-10-01|title=The evolutionary nature of RV Tauri stars in the SMC and LMC|bibcode=2018A&A...618A..21M|journal=Astronomy and Astrop ...rs discovered in the UKST Hα survey of the Large Magellanic Cloud - I. Hot stars |author1=Reid, Warren A. |author2=Parker, Quentin A. |journal=Monthly Notic ...4 KB (508 words) - 03:48, 3 October 2024
- ...s|the most massive]] and [[List of most luminous stars|most luminous known stars]].<ref name=wu/> ...pectral type of O2-3.5If<sup>*</sup>. The star is one of the most luminous stars known, with a luminosity of {{solar luminosity|4,365,000}}, and has a tempe ...4 KB (599 words) - 14:56, 9 October 2024
- ...iv = astro-ph/0301257 }}</ref> is the radius at which the enclosed mass in stars equals twice ''M''<sub>BH</sub>, i.e. ...inition compares the force from the black hole to the local force from the stars. ...4 KB (612 words) - 08:42, 9 November 2024
- ...r absorption coefficients and opacities|title= Stellar Structure |series= Stars and Stellar Systems: Compendium of Astronomy and Astrophysics |volume=VIII| ...ömgren|title=The opacity of stellar matter and the hydrogen content of the stars|journal=Zeitschrift für Astrophysik|date=1932|volume=4|pages=118–152|bibcod ...2 KB (251 words) - 04:49, 16 December 2023
- ...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 ...4 KB (602 words) - 05:15, 18 November 2024
- * [[Mercury-manganese star]], a class of chemically peculiar stars ...710 bytes (91 words) - 01:37, 24 May 2024
- ...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 ...5 KB (791 words) - 05:22, 17 November 2024
- * [[Ap star]], a class of chemically-peculiar stars ...787 bytes (99 words) - 17:46, 15 January 2022
- * [[Am star]], a class of chemically-peculiar stars ...783 bytes (109 words) - 09:22, 17 February 2025
- ...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 ...6 KB (866 words) - 17:47, 25 September 2024
- ...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 ...6 KB (793 words) - 16:49, 18 July 2024
- The angle brackets denote averages over the ensemble of observed stars. {{math|''M''(''r'')}} is the mass contained within a distance {{mvar|r}} f # the mass is distributed in the same way as the observed stars. ...4 KB (593 words) - 08:47, 13 December 2024
- {{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. ...4 KB (586 words) - 20:26, 19 May 2024
- ...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 ...e Jump Cannon|Annie Jump Cannon's]] 1907 work ''Second Catalog of Variable Stars''.<ref name="Cannon1907"/> ...6 KB (782 words) - 01:33, 31 December 2024