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{{Short description|Measure of the strength of a spectral line}} ...|A diagram indicating the equivalent width corresponding to the absorption line, which is shown in red.]] ...

...n]]s.<ref>{{cite journal |title = Near-infrared observations of the carbon stars TU Geminorum and SS Virginis at milliarcsecond resolution |last1 = Richichi ...esolve?urn=urn:nbn:se:uu:diva-423949 |title=Dust emission modelling of AGB stars |date=2020}}</ref> ...

...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 ...urth US Naval Observatory CCD Astrograph Catalog (UCAC4)|journal=VizieR On-line Data Catalog|date=2012|bibcode=2012yCat.1322....0Z}}</ref> ...

...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 ...

R Volantis' peculiarity was first observed in 1954 when it was found to have emission lines in its spectrum.<ref name = Bidelman1954/> Observations from 1955 to ...]] of Ce,<ref name="Henize1976"/> indicating that it is a carbon star with emission lines. It is a giant star on the [[asymptotic giant branch]],<ref name = Mo ...

...nown as '''V1104 Scorpii''', is a binary star containing a unique emission-line star, which is in the midst of transitioning to a nitrogen-rich [[Wolf–Raye ...suggests a large [[circumbinary]] disk, which is the source of stationary emission lines in the spectrum. The complex light curve is probably due to the tidal ...

...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 ...

...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 ...

...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"/> ...

...also called the spin temperature, of neutral [[hydrogen]] to [[Lyman-alpha line|Lyman-alpha]] radiation. This coupling plays a role in producing a differen ...ly when the two temperatures differ, i.e. are decoupled, that the hydrogen line can be observed.<ref>Stiavelli (2009), p. 121.</ref> ...

...0271 |title=Harvard College Observatory, circular no. 10. Six new variable stars |year=1896 |last1=Pickering |first1=E. C. |last2=Leland |first2=E. F. |jour ...ibcode=2001A&A...369..178B|title=The effective temperatures of carbon-rich stars|journal=Astronomy and Astrophysics|volume=369|pages=178–209|last1=Bergeat|f ...

...ral line|line]].<ref name="Knapp"/> Later studies of millimeter-wave radio emission have detected over 20 different molecular species in the CSE. There include ...esolution [[Interferometry|interferometric]] measurements show that the CO emission lines arise from a spiral structure. The spiral structure of the molecular ...

...atomic hydrogen gas became ionised due to ultraviolet light from the first stars. ...t from the first stars in the Universe altering the emission of the [[21cm line]] by lowering the temperature of the hydrogen relative to the [[cosmic micr ...

...an O’Donnell|epoch=[[Epoch (astronomy)#Julian years and J2000|J2000]]|type=emission|type2=[[Superbubble]]|ra={{RA|05|43|17.5}}<ref name="nebula"/>|dec={{DEC|-6 '''Henize 70''' ('''N70''') is a faint<ref name="pn" /> [[emission nebula]]<ref name="henize" /> and [[superbubble]]<ref name="apod" /><ref na ...

...ss of "WR + ABS".<ref name=gosset/><ref name=wr6/> A review of Wolf-Rayet stars in 1984 reported that WR 30a had a [[right ascension]] greater than [[WR 30 ...O{{smallcaps|vi}} emission but confirmed by the lack of C{{smallcaps|iii}} emission. A WO5 class was temporarily assigned to account for the unusually low exc ...

...e instrument for each imaged object. For distributed objects with emission-line spectra (such as the Sun in [[extreme ultraviolet]]), it results in an imag ...th>\lambda</math> is the wavelength of interest, and <math>D</math> is the line spacing of the grating. Because the [[sine]] function (and its inverse) are ...

...gue of Stellar Spectral Classifications (Skiff, 2009- ) |journal=VizieR On-line Data Catalog |last1=Skiff |first1=B. A. |year=2014 }}</ref> ...: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S|volume=1 ...

{{short description|Light from the stars}} ...refers to [[visible spectrum|visible]] [[electromagnetic radiation]] from stars other than the [[Sun]], observable from [[Earth]] at [[night]], although a ...

...cted by this mission is expected to shed light on the genesis of the first stars, the rapid growth of the initial black holes,<ref>{{Cite journal |last1=Ale |title= Probing the first stars and black holes in the early Universe with the Dark Ages Radio Explorer (DA ...

...[[ionised]] [[helium]] found, usually in absorption, in the spectra of hot stars like [[Wolf–Rayet star]]s. The name comes from [[Edward Charles Pickering]] ...er, they are seen in emission in the spectra of Wolf-Rayet stars, as these stars have little or no hydrogen. ...