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Micron Document

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</style><div id="coordinates" class="coordinates"><a class="external text" href="https://geohack.toolforge.org/skyhack.php?ra=20.341104466667&de=43.854522277778&size=0.0033333333333333&name=WR+140&object=WR%20140&_globe:=">Datenbanklinks zu WR 140</a></div>

<th colspan="2" class="ibheader"><a href="Stern" title="Stern">Stern</a><br> WR 140

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<td colspan="2" class="ibimgtxt">Die Staubschalen um WR140, aufgenommen mithilfe des <a href="James-Webb-Weltraumteleskop" title="James-Webb-Weltraumteleskop">James-Webb-Weltraumteleskops</a>

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<td colspan="2" style="text-align:center;"><a rel="nofollow" class="external text" href="https://aladin.cds.unistra.fr/AladinLite/?target=20%2020%2027.97608%20%2B43%2051%2016.2802&fov=0.005&survey=CDS%2FP%2FDSS2%2Fcolor">AladinLite</a>

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<th colspan="2" class="ibheader">Beobachtungsdaten<br><small><a href="%C3%84quinoktium" title="Äquinoktium">Äquinoktium</a>: <a href="Epoche_(Astronomie)#Standardepochen" title="Epoche (Astronomie)">J2000.0</a>, <a href="Epoche_(Astronomie)" title="Epoche (Astronomie)">Epoche</a>: J2000.0</small>

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<td><a href="Sternbild" title="Sternbild">Sternbild</a>

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<td class="ibnowrap"><a href="Schwan_(Sternbild)" title="Schwan (Sternbild)">Schwan</a>

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<td><a href="Rektaszension" title="Rektaszension">Rektaszension</a>

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<td><a href="Deklination_(Astronomie)" title="Deklination (Astronomie)">Deklination</a>

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<td><a href="Scheinbare_Gr%C3%B6%C3%9Fe" title="Scheinbare Größe">Winkelausdehnung</a>

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<td class="ibnowrap">{{{Winkel}}} <a href="Winkelsekunde" title="Winkelsekunde">mas</a>

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<td>Bekannte <a href="Exoplanet" title="Exoplanet">Exoplaneten</a>

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<th colspan="2" class="ibheader">Helligkeiten

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<td><a href="Scheinbare_Helligkeit" title="Scheinbare Helligkeit">Scheinbare Helligkeit</a>

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<td class="ibnowrap"> mag

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<td><a href="UBV-System" title="UBV-System">Helligkeit (U-Band)</a>

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<td class="ibnowrap"> mag

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<td><a href="UBV-System" title="UBV-System">Helligkeit (B-Band)</a>

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<td class="ibnowrap"> mag

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<td><a href="UBV-System" title="UBV-System">Helligkeit (V-Band)</a>

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<td><a href="UBV-System#Erweiterungen" title="UBV-System">Helligkeit (R-Band)</a>

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<td class="ibnowrap"> mag

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<td><a href="UBV-System#Erweiterungen" title="UBV-System">Helligkeit (I-Band)</a>

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<td class="ibnowrap"> mag

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<td><a href="Frequenzband#Astronomie" title="Frequenzband">Helligkeit (J-Band)</a>

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<td class="ibnowrap"> mag

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<td><a href="Frequenzband#Astronomie" title="Frequenzband">Helligkeit (H-Band)</a>

</td>

<td class="ibnowrap"> mag

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<td><a href="Frequenzband#Astronomie" title="Frequenzband">Helligkeit (K-Band)</a>

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<td class="ibnowrap"> mag

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<td><a href="G-Band-Magnitude" title="G-Band-Magnitude">G-Band-Magnitude</a>

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<td class="ibnowrap"> mag

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<th colspan="2" class="ibheader">Spektrum und Indices

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<td><a href="Benennung_ver%C3%A4nderlicher_Sterne" title="Benennung veränderlicher Sterne">Veränderlicher Sterntyp</a>

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<td>B−V-Farbindex

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<td>U−B-<a href="Farbindex" title="Farbindex">Farbindex</a>

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<td>R−I-Index

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<td><a href="Spektralklasse" title="Spektralklasse">Spektralklasse</a>

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<th colspan="2" class="ibheader"><a href="Astrometrie" title="Astrometrie">Astrometrie</a>

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<td><a href="Radialgeschwindigkeit" title="Radialgeschwindigkeit">Radialgeschwindigkeit</a>

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<td><a href="Parallaxe" title="Parallaxe">Parallaxe</a>

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<td>Entfernung

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<td>Visuelle <a href="Absolute_Helligkeit" title="Absolute Helligkeit">Absolute Helligkeit</a> M<sub>vis</sub>

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<td class="ibnowrap"> mag

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<td>Bolometrische <a href="Absolute_Helligkeit" title="Absolute Helligkeit">Absolute Helligkeit</a> M<sub>bol</sub>

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<td class="ibnowrap">{{{Absolut-bol}}} mag

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<th colspan="2" class="ibheader"><a href="Eigenbewegung_(Astronomie)" title="Eigenbewegung (Astronomie)">Eigenbewegung</a>

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<td>Rek.-Anteil:

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<td>Dekl.-Anteil:

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<th colspan="2" class="ibheader">Physikalische Eigenschaften

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<td><a href="Masse_(Physik)" title="Masse (Physik)">Masse</a>

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<td><a href="Radius" title="Radius">Radius</a>

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<td><a href="Leuchtkraft" title="Leuchtkraft">Leuchtkraft</a>

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<td><a href="Effektive_Temperatur" title="Effektive Temperatur">Effektive Temperatur</a>

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<td><a href="Metallizit%C3%A4t" title="Metallizität">Metallizität</a> [Fe/H]

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<td><a href="Sternrotation" title="Sternrotation">Rotationsdauer</a>

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<td>Alter

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<th colspan="2" class="ibheader">Andere Bezeichnungen und <a href="Liste_astronomischer_Kataloge" title="Liste astronomischer Kataloge">Katalogeinträge</a>

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<td colspan="2"><table class="centered" style="width:100%; border:none; font-size:smaller; margin:0 .2em; white-space:nowrap; line-height:1.3em;"><tbody><tr><td style="white-space:nowrap;"><a href="Bonner_Durchmusterung" title="Bonner Durchmusterung">Bonner Durchmusterung</a></td><td style="white-space:nowrap;">BD +43°3571</td></tr><tr><td style="white-space:nowrap;"><a href="Henry-Draper-Katalog" title="Henry-Draper-Katalog">Henry-Draper-Katalog</a></td><td style="white-space:nowrap;">HD 193793 <a rel="nofollow" class="external autonumber" href="https://cdsarc.u-strasbg.fr/viz-bin/VizieR-5?-source=III/135A/catalog&-out.all&-out.max=10&HD==193793">[1]</a></td></tr><tr><td style="white-space:nowrap;"><a href="Hipparcos-Katalog" title="Hipparcos-Katalog">Hipparcos-Katalog</a></td><td style="white-space:nowrap;">HIP 100287 <a rel="nofollow" class="external autonumber" href="https://vizier.u-strasbg.fr/viz-bin/VizieR-5?-source=I/311&-out.all&-out.max=10&HIP==100287">[2]</a></td></tr><tr><td style="white-space:nowrap;"><a href="Tycho-1-Katalog" title="Tycho-1-Katalog">Tycho-Katalog</a></td><td style="white-space:nowrap;">TYC 3164-1678-1<a rel="nofollow" class="external autonumber" href="https://cdsarc.u-strasbg.fr/viz-bin/VizieR-5?-source=I/259&-out.all&-out.max=100&TYC1=3164&TYC2=1678&TYC3=1">[3]</a><span style="display:none">Vorlage:Infobox Stern/Wartung/AngabeTYC-Katalog</span></td></tr><tr><td style="white-space:nowrap;"><a href="Two_Micron_All_Sky_Survey" title="Two Micron All Sky Survey">2MASS-Katalog</a></td><td style="white-space:nowrap;">2MASS J20202798+4351164<a rel="nofollow" class="external autonumber" href="https://vizier.u-strasbg.fr/viz-bin/VizieR-5?-source=II/246/out&-out.all&&-out.max=10&2MASS=20202798%2B4351164">[4]</a></td></tr><tr><td style="white-space:nowrap; vertical-align:top; padding-top:0.2em;">Weitere Bezeichnungen</td><td style="white-space:normal;">

V1687 Cygni • SBC9 1232 • <a href="Washington_Double_Star_Catalog" title="Washington Double Star Catalog">WDS</a> J20205+4351</td></tr></tbody></table>

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<th colspan="2" class="ibheader">Anmerkung

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<td colspan="2">{{{Anmerkung}}}

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<p><b>WR 140</b> ist ein <a href="Wolf-Rayet-Stern" title="Wolf-Rayet-Stern">Wolf-Rayet-Stern</a>, der zusammen mit einem Stern der <a href="Klassifizierung_der_Sterne#Spektraltypen_durch_Spektren" title="Klassifizierung der Sterne">Spektralklasse O4-5</a> ein <a href="Doppelsternsystem" class="mw-redirect" title="Doppelsternsystem">Doppelsternsystem</a> (<b>SBC9 1232)</b><sup id="cite_ref-sb9_4-0" class="reference"><a href="#cite_note-sb9-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> im <a href="Schwan_(Sternbild)" title="Schwan (Sternbild)">Sternbild Schwan</a> bildet. Das System ein hervorragendes Beispiel für eine phasenweise Staubproduktion, bei dem aus dem <a href="Silicium" title="Silicium">silicium</a>- und <a href="Kohlenstoff" title="Kohlenstoff">kohlenstoffhaltigen</a><sup id="cite_ref-roe_5-0" class="reference"><a href="#cite_note-roe-5"><span class="cite-bracket">[</span>5<span class="cite-bracket">]</span></a></sup> <a href="Sternwind" title="Sternwind">Sternwind</a> von WR 140 kondensierter <a href="Kosmischer_Staub" title="Kosmischer Staub">kosmischen Staub</a> verschachtelte Staubhüllen entstehen<sup id="cite_ref-moffat_6-0" class="reference"><a href="#cite_note-moffat-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-monnier_7-0" class="reference"><a href="#cite_note-monnier-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup> – im Unterschied zu beispielsweise <a href="WR_104" title="WR 104">WR 104</a>, bei dem eine spiralförmige Staubverteilung auftritt.

</p><p>WR 140 ist einer der hellsten Wolf-Rayet-Sterne des <a href="Nordhimmel" title="Nordhimmel">Nordhimmels</a>. Dennoch ist er masseärmer und weniger leuchtstark als der primäre Stern des Doppelsternsystems, überstrahlt aber dessen Spektrum mit seinen breiten <a href="Spektrallinie" title="Spektrallinie">Spektrallinien</a>. Der primäre Stern ist ein <a href="Riesenstern" title="Riesenstern">Riesenstern</a> oder <a href="%C3%9Cberriese" class="mw-redirect" title="Überriese">Überriese</a>. Spektroskopisch konnte ein stark exzentrischer Orbit mit einer <a href="Umlaufzeit" title="Umlaufzeit">Umlaufzeit</a> von 7,9 ± 0,2 Jahren bestimmt werden: Der Abstand beider Sterne variiert von 1,3 <a href="Astronomische_Einheit" title="Astronomische Einheit">AU</a> im <a href="Periastron" class="mw-redirect" title="Periastron">Periastron</a> bis hin zu 23,9 AU im Apastron. Kurz nach der Periastron-Passage alle 8 Jahre steigt die Infrarotemission stark an und fällt dann über einen Zeitraum von mehreren Monaten wieder ab. In dieser Phase kollidieren <a href="Sternwind" title="Sternwind">Sternwind</a> und die von dem Wolf-Rayet-Stern entstehenden Staubpartikel. Es ist allerdings noch nicht geklärt (Stand 2022), ob die besondere, konzentrische Struktur der Staubschalen durch die Interaktion der beiden Sternwinde hervorgerufen wird oder das Ergebnis von Prozessen im Kern des Wolf-Rayet-Sterns sind.<sup id="cite_ref-episodic_8-0" class="reference"><a href="#cite_note-episodic-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup>

</p><p>Die Oberflächentemperatur des Wolf-Rayet-Sterns beträgt 70.000 <a href="Kelvin" title="Kelvin">Kelvin</a>, die des Primärsterns 35.000 Kelvin.<sup id="cite_ref-williams_9-0" class="reference"><a href="#cite_note-williams-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup> Sie erzeugen eine energiereiche <a href="Ultraviolettstrahlung" title="Ultraviolettstrahlung">Ultraviolettstrahlung</a> und erhitzen die Staubschalen auf eine Temperatur von etwa 1.000 Kelvin, so dass rund 20 Lagen im Infrarotspektrum sichtbar werden. Der Abstand der konzentrischen Schalen beträgt etwa 1,4 <a href="Billion" title="Billion">Billionen</a> km (1,4·10<sup>12</sup> km), das entspricht 3,5 % des Abstands zwischen Sonne und <a href="Alpha_Centauri" title="Alpha Centauri">Alpha Centauri</a>.<sup id="cite_ref-twitter_10-0" class="reference"><a href="#cite_note-twitter-10"><span class="cite-bracket">[</span>10<span class="cite-bracket">]</span></a></sup>

</p>

<div class="mw-heading mw-heading2"><h2 id="Literatur">Literatur</h2></div>

<ul><li>Joshua D. Thomas et al.: <cite style="font-style:italic">The orbit and stellar masses of the archetype colliding-wind binary WR 140</cite>. In: <cite style="font-style:italic"><a href="Monthly_Notices_of_the_Royal_Astronomical_Society" title="Monthly Notices of the Royal Astronomical Society">Monthly Notices of the Royal Astronomical Society</a></cite>. 504. Jahrgang, <span style="white-space:nowrap">Nr.<span style="display:inline-block;width:.2em"> </span>4</span>, 2021, <span style="white-space:nowrap">S.<span style="display:inline-block;width:.2em"> </span>5221–5230</span>, <a href="Digital_Object_Identifier" title="Digital Object Identifier">doi</a>:<span class="uri-handle" style="white-space:nowrap"><a rel="nofollow" class="external text" href="https://doi.org/10.1093/mnras%2Fstab1181">10.1093/mnras/stab1181</a></span>, <a href="ArXiv" title="ArXiv">arxiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/2101.10563">2101.10563</a>.<span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rfr_id=info:sid/de.wikipedia.org:WR+140&rft.atitle=The+orbit+and+stellar+masses+of+the+archetype+colliding-wind+binary+WR+140&rft.au=Joshua+D.+Thomas+et+al.&rft.date=2021&rft.doi=10.1093%2Fmnras%2Fstab1181&rft.genre=journal&rft.issue=4&rft.jtitle=Monthly+Notices+of+the+Royal+Astronomical+Society&rft.pages=5221-5230&rft.volume=504.+Jahrgang" style="display:none"> </span></li>

<li>Ryan M. Lau et al.: <cite style="font-style:italic">Nested dust shells around the Wolf–Rayet binary WR 140 observed with JWST</cite>. In: <cite style="font-style:italic"><a href="Nature_Astronomy" class="mw-redirect" title="Nature Astronomy">Nature Astronomy</a></cite>. 2022, <a href="Digital_Object_Identifier" title="Digital Object Identifier">doi</a>:<span class="uri-handle" style="white-space:nowrap"><a rel="nofollow" class="external text" href="https://doi.org/10.1038/s41550-022-01812-x">10.1038/s41550-022-01812-x</a></span>.<span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rfr_id=info:sid/de.wikipedia.org:WR+140&rft.atitle=Nested+dust+shells+around+the+Wolf-Rayet+binary+WR+140+observed+with+JWST&rft.au=Ryan+M.+Lau+et+al.&rft.btitle=Nature+Astronomy&rft.date=2022&rft.doi=10.1038%2Fs41550-022-01812-x&rft.genre=book" style="display:none"> </span></li></ul>

<div class="mw-heading mw-heading2"><h2 id="Einzelnachweise">Einzelnachweise</h2></div>

<li id="cite_note-hipparcos-1"><span class="mw-cite-backlink"><a href="#cite_ref-hipparcos_1-0">↑</a></span> <span class="reference-text">F. Van Leeuwen: <cite style="font-style:italic">Validation of the new Hipparcos reduction</cite>. In: <cite style="font-style:italic"><a href="Astronomy_and_Astrophysics" class="mw-redirect" title="Astronomy and Astrophysics">Astronomy and Astrophysics</a></cite>. 474. Jahrgang, <span style="white-space:nowrap">Nr.<span style="display:inline-block;width:.2em"> </span>2</span>, 2007, <span style="white-space:nowrap">S.<span style="display:inline-block;width:.2em"> </span>653–664</span>, <a href="Digital_Object_Identifier" title="Digital Object Identifier">doi</a>:<span class="uri-handle" style="white-space:nowrap"><a rel="nofollow" class="external text" href="https://doi.org/10.1051/0004-6361%3A20078357">10.1051/0004-6361:20078357</a></span>, <a href="ArXiv" title="ArXiv">arxiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/0708.1752">0708.1752</a>, <a href="Bibcode" title="Bibcode">bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2007A&A...474..653V">2007A&A...474..653V</a>.<span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rfr_id=info:sid/de.wikipedia.org:WR+140&rft.atitle=Validation+of+the+new+Hipparcos+reduction&rft.au=F.%26%2332%3BVan+Leeuwen&rft.date=2007&rft.doi=10.1051%2F0004-6361%3A20078357&rft.genre=journal&rft.issue=2&rft.jtitle=Astronomy+and+Astrophysics&rft.pages=653-664&rft.volume=474.+Jahrgang" style="display:none"> </span></span>

</li>

<li id="cite_note-ducati-2"><span class="mw-cite-backlink"><a href="#cite_ref-ducati_2-0">↑</a></span> <span class="reference-text">J. R. Ducati: <cite style="font-style:italic">VizieR On-Line Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system</cite>. In: <cite style="font-style:italic">CDS/ADC Collection of Electronic Catalogues</cite>. 2237. Jahrgang, 2002, <a href="Bibcode" title="Bibcode">bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2002yCat.2237....0D">2002yCat.2237....0D</a>.<span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rfr_id=info:sid/de.wikipedia.org:WR+140&rft.atitle=VizieR+On-Line+Data+Catalog%3A+Catalogue+of+Stellar+Photometry+in+Johnson%27s+11-color+system&rft.au=J.+R.%26%2332%3BDucati&rft.btitle=CDS%2FADC+Collection+of+Electronic+Catalogues&rft.date=2002&rft.genre=book&rft.volume=2237.+Jahrgang" style="display:none"> </span></span>

</li>

<li id="cite_note-rv-3"><span class="mw-cite-backlink"><a href="#cite_ref-rv_3-0">↑</a></span> <span class="reference-text">D. Pourbaix, A. A. Tokovinin, A. H. Batten, F. C. Fekel, W. I. Hartkopf, H. Levato, N. I. Morrell, G. Torres, S. Udry: <cite style="font-style:italic">SB9: The ninth catalogue of spectroscopic binary orbits</cite>. In: <cite style="font-style:italic"><a href="Astronomy_and_Astrophysics" class="mw-redirect" title="Astronomy and Astrophysics">Astronomy and Astrophysics</a></cite>. 424. Jahrgang, <span style="white-space:nowrap">Nr.<span style="display:inline-block;width:.2em"> </span>2</span>, 2004, <span style="white-space:nowrap">S.<span style="display:inline-block;width:.2em"> </span>727–732</span>, <a href="Digital_Object_Identifier" title="Digital Object Identifier">doi</a>:<span class="uri-handle" style="white-space:nowrap"><a rel="nofollow" class="external text" href="https://doi.org/10.1051/0004-6361%3A20041213">10.1051/0004-6361:20041213</a></span>, <a href="ArXiv" title="ArXiv">arxiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/astro-ph/0406573">astro-ph/0406573</a>, <a href="Bibcode" title="Bibcode">bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2004A&A...424..727P">2004A&A...424..727P</a>.<span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rfr_id=info:sid/de.wikipedia.org:WR+140&rft.atitle=SB9%3A+The+ninth+catalogue+of+spectroscopic+binary+orbits&rft.au=D.%26%2332%3BPourbaix%2C%26%2332%3BA.+A.%26%2332%3BTokovinin%2C%26%2332%3BA.+H.%26%2332%3BBatten%2C+...&rft.date=2004&rft.doi=10.1051%2F0004-6361%3A20041213&rft.genre=journal&rft.issue=2&rft.jtitle=Astronomy+and+Astrophysics&rft.pages=727-732&rft.volume=424.+Jahrgang" style="display:none"> </span></span>

</li>

<li id="cite_note-sb9-4"><span class="mw-cite-backlink"><a href="#cite_ref-sb9_4-0">↑</a></span> <span class="reference-text">D. Pourbaix, S. Udry: <cite style="font-style:italic">VizieR Online Data Catalog: SB9: 9th Catalogue of Spectroscopic Binary Orbits (Pourbaix+ 2004-2014)</cite>. In: <cite style="font-style:italic">VizieR On-Line Data Catalog: B/Sb9. Originally Published in: 2004A&A...424..727P</cite>. 1. Jahrgang, 2004, <span style="white-space:nowrap">S.<span style="display:inline-block;width:.2em"> </span>727–732</span>, <a href="Digital_Object_Identifier" title="Digital Object Identifier">doi</a>:<span class="uri-handle" style="white-space:nowrap"><a rel="nofollow" class="external text" href="https://doi.org/10.1051/0004-6361%3A20041213">10.1051/0004-6361:20041213</a></span>, <a href="ArXiv" title="ArXiv">arxiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/astro-ph/0406573">astro-ph/0406573</a>, <a href="Bibcode" title="Bibcode">bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2004A&A...424..727P">2004A&A...424..727P</a>.<span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rfr_id=info:sid/de.wikipedia.org:WR+140&rft.atitle=VizieR+Online+Data+Catalog%3A+SB9%3A+9th+Catalogue+of+Spectroscopic+Binary+Orbits+%28Pourbaix%2B+2004-2014%29&rft.au=D.%26%2332%3BPourbaix%2C%26%2332%3BS.%26%2332%3BUdry&rft.btitle=VizieR+On-Line+Data+Catalog%3A+B%2FSb9.+Originally+Published+in%3A+2004A%26A...424..727P&rft.date=2004&rft.doi=10.1051%2F0004-6361%3A20041213&rft.genre=book&rft.pages=727-732&rft.volume=1.+Jahrgang" style="display:none"> </span></span>

</li>

<li id="cite_note-roe-5"><span class="mw-cite-backlink"><a href="#cite_ref-roe_5-0">↑</a></span> <span class="reference-text"><span class="cite"><a rel="nofollow" class="external text" href="https://www.roe.ac.uk/~pmw/Wr140int.htm"><i>WR140 Introduction.</i></a> In: <i>www.roe.ac.uk.</i><span class="Abrufdatum"> Abgerufen am 29. August 2022</span>.</span><span style="display: none;" class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Adc&rfr_id=info%3Asid%2Fde.wikipedia.org%3AWR+140&rft.title=WR140+Introduction&rft.description=WR140+Introduction&rft.identifier=&rft.date="> </span></span>

</li>

<li id="cite_note-moffat-6"><span class="mw-cite-backlink"><a href="#cite_ref-moffat_6-0">↑</a></span> <span class="reference-text">A. F. J. Moffat, M. M. Shara: <cite style="font-style:italic">Photometric variability of a complete sample of northern Wolf-Rayet stars</cite>. In: <cite style="font-style:italic"><a href="Astronomical_Journal" title="Astronomical Journal">Astronomical Journal</a></cite>. 92. Jahrgang, 1986, <span style="white-space:nowrap">S.<span style="display:inline-block;width:.2em"> </span>952</span>, <a href="Digital_Object_Identifier" title="Digital Object Identifier">doi</a>:<span class="uri-handle" style="white-space:nowrap"><a rel="nofollow" class="external text" href="https://doi.org/10.1086/114227">10.1086/114227</a></span>, <a href="Bibcode" title="Bibcode">bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1986AJ.....92..952M">1986AJ.....92..952M</a>.<span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rfr_id=info:sid/de.wikipedia.org:WR+140&rft.atitle=Photometric+variability+of+a+complete+sample+of+northern+Wolf-Rayet+stars&rft.au=A.+F.+J.%26%2332%3BMoffat%2C%26%2332%3BM.+M.%26%2332%3BShara&rft.btitle=Astronomical+Journal&rft.date=1986&rft.doi=10.1086%2F114227&rft.genre=book&rft.pages=952&rft.volume=92.+Jahrgang" style="display:none"> </span></span>

</li>

<li id="cite_note-monnier-7"><span class="mw-cite-backlink"><a href="#cite_ref-monnier_7-0">↑</a></span> <span class="reference-text">J. D. Monnier, Ming Zhao, E. Pedretti, R. Millan-Gabet, J.-P. Berger, W. Traub, F. P. Schloerb, T. Ten Brummelaar, H. McAlister, S. Ridgway, L. Sturmann, J. Sturmann, N. Turner, F. Baron, S. Kraus, A. Tannirkulam, P. M. Williams: <cite style="font-style:italic">First Visual Orbit for the Prototypical Colliding-wind Binary WR 140</cite>. In: <cite style="font-style:italic">The Astrophysical Journal Letters</cite>. 742. Jahrgang, <span style="white-space:nowrap">Nr.<span style="display:inline-block;width:.2em"> </span>1</span>, 2011, <span style="white-space:nowrap">S.<span style="display:inline-block;width:.2em"> </span>L1</span>, <a href="Digital_Object_Identifier" title="Digital Object Identifier">doi</a>:<span class="uri-handle" style="white-space:nowrap"><a rel="nofollow" class="external text" href="https://doi.org/10.1088/2041-8205%2F742%2F1%2FL1">10.1088/2041-8205/742/1/L1</a></span>, <a href="ArXiv" title="ArXiv">arxiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/1111.1266">1111.1266</a>, <a href="Bibcode" title="Bibcode">bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2011ApJ...742L...1M">2011ApJ...742L...1M</a>.<span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rfr_id=info:sid/de.wikipedia.org:WR+140&rft.atitle=First+Visual+Orbit+for+the+Prototypical+Colliding-wind+Binary+WR+140&rft.au=J.+D.%26%2332%3BMonnier%2C%26%2332%3BMing%26%2332%3BZhao%2C%26%2332%3BE.%26%2332%3BPedretti%2C+...&rft.date=2011&rft.doi=10.1088%2F2041-8205%2F742%2F1%2FL1&rft.genre=journal&rft.issue=1&rft.jtitle=The+Astrophysical+Journal+Letters&rft.pages=L1&rft.volume=742.+Jahrgang" style="display:none"> </span></span>

</li>

<li id="cite_note-episodic-8"><span class="mw-cite-backlink"><a href="#cite_ref-episodic_8-0">↑</a></span> <span class="reference-text"><span class="cite"><a rel="nofollow" class="external text" href="https://www.roe.ac.uk/~pmw/Wr140edm.htm"><i>Episodic (and variable) dust-making WR stars.</i></a> In: <i>www.roe.ac.uk.</i><span class="Abrufdatum"> Abgerufen am 2. September 2022</span>.</span><span style="display: none;" class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Adc&rfr_id=info%3Asid%2Fde.wikipedia.org%3AWR+140&rft.title=Episodic+%28and+variable%29+dust-making+WR+stars&rft.description=Episodic+%28and+variable%29+dust-making+WR+stars&rft.identifier=&rft.date="> </span></span>

</li>

<li id="cite_note-williams-9"><span class="mw-cite-backlink"><a href="#cite_ref-williams_9-0">↑</a></span> <span class="reference-text">Peredur Williams: <cite style="font-style:italic">Results from the 2009 campaign on WR 140</cite>. In: <cite style="font-style:italic">Société Royale des Sciences de Liège</cite>. 80. Jahrgang, 2011, <span style="white-space:nowrap">S.<span style="display:inline-block;width:.2em"> </span>595</span>, <a href="Bibcode" title="Bibcode">bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2011BSRSL..80..595W">2011BSRSL..80..595W</a>.<span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rfr_id=info:sid/de.wikipedia.org:WR+140&rft.atitle=Results+from+the+2009+campaign+on+WR+140&rft.au=Peredur%26%2332%3BWilliams&rft.btitle=Soci%C3%A9t%C3%A9+Royale+des+Sciences+de+Li%C3%A8ge&rft.date=2011&rft.genre=book&rft.pages=595&rft.volume=80.+Jahrgang" style="display:none"> </span></span>

</li>

<li id="cite_note-twitter-10"><span class="mw-cite-backlink"><a href="#cite_ref-twitter_10-0">↑</a></span> <span class="reference-text"><span class="cite">Mark McCaughrean: <a rel="nofollow" class="external text" href="https://twitter.com/markmccaughrean/status/1564229429949353988"><i>Surprised no-one spotted my awful maths yet.</i></a> In: <i>Twitter.</i><span class="Abrufdatum"> Abgerufen am 2. September 2022</span> (englisch).</span><span style="display: none;" class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Adc&rfr_id=info%3Asid%2Fde.wikipedia.org%3AWR+140&rft.title=Surprised+no-one+spotted+my+awful+maths+yet&rft.description=Surprised+no-one+spotted+my+awful+maths+yet&rft.identifier=&rft.creator=Mark+McCaughrean&rft.date=&rft.language=en"> </span></span>

</li>

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