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Revision as of 22:26, 30 March 2024 edit2002:8919:eec9:0:4067:169f:5580:a136 (talk) Added discovery of outbursts in 1217 and 1787.Tags: Reverted Visual edit← Previous edit Latest revision as of 10:24, 12 December 2024 edit undoMortense (talk | contribs)Extended confirmed users11,769 editsm →2016–present activity: Copy edited. 
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}} }}
{{Starbox catalog {{Starbox catalog
|names={{odlist|AAVSO=1555+26|2MASS=J15593015+2555126|HD=143454|HR=5958|BD=+26° 2765|HIP=78322|SAO=84129}}, T Cor Bor<ref>{{Cite journal |last1=Starrfield |first1=Sumner |last2=Bose |first2=Maitrayee |last3=Woodward |first3=Charles E. |last4=Perron |first4=Isabelle |last5=Shaw |first5=Gargi |last6=Evans |first6=Aneurin |last7=Iliadis |first7=Christian |last8=Hix |first8=W. Raphael |date=2024-06-01 |title=The evolution leading to a thermonuclear runaway |bibcode=2024AAS...24413201S |journal=Bulletin of the American Astronomical Society |volume=56 |issue=7 |pages=132.01}}</ref>
|names={{odlist|AAVSO=1555+26|2MASS=J15593015+2555126|HD=143454|BD=+26° 2765|HIP=78322|SAO=84129}}
}} }}
{{Starbox reference {{Starbox reference
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'''T Coronae Borealis''' (''T CrB''), is a recurrent ] in the ] ].<ref name="NYT-20240308">{{cite news |last=Andrews |first=Robin George |title=The Night Sky Will Soon Get ‘a New Star.’ Here’s How to See It. - A nova named T Coronae Borealis lit up the night about 80 years ago, and astronomers say it’s expected to put on another show in the coming months. |url=https://www.nytimes.com/article/nova-new-star-t-coronae-borealis.html |date=8 March 2024 |work=] |url-status=live |archiveurl=https://archive.today/20240308220630/https://www.nytimes.com/article/nova-new-star-t-coronae-borealis.html|archivedate=8 March 2024 |accessdate=9 March 2024 }}</ref> It was first discovered in outburst in 1866 by ],<ref name=pettit>{{cite journal|bibcode=1946PASP...58..153P|title=The Light-Curves of T Coronae Borealis|journal=Publications of the Astronomical Society of the Pacific|volume=58|pages=153|last1=Pettit|first1=Edison|year=1946|issue=341|doi=10.1086/125797|doi-access=free}}</ref> although it had been observed earlier as a 10th magnitude star.<ref name=barnard>{{cite journal|bibcode=1907ApJ....25..279B|title=Nova T Coronae of 1866|journal=Astrophysical Journal|volume=25|pages=279|last1=Barnard|first1=E. E.|year=1907|doi=10.1086/141446}}</ref> It may have been observed in 1217 and in 1787 as well.<ref>{{cite web |title=The recurrent nova T CrB had prior eruptions observed near December 1787 and October 1217 AD |publisher=Journal for the History of Astronomy |url=https://journals.sagepub.com/doi/abs/10.1177/00218286231200492 |accessdate=2024-03-21}}</ref><ref>{{cite web |title=Evidence of mysterious 'recurring nova' that could reappear in 2024 found in medieval manuscript from 1217 |publisher=Live Science |url=https://www.livescience.com/space/astronomy/evidence-of-mysterious-recurring-nova-that-could-reappear-in-2024-found-in-medieval-manuscript-from-1217 |accessdate=2024-03-21}}</ref> '''T Coronae Borealis''' (''T CrB''), nicknamed the '''Blaze Star''', is a ] and a recurrent ] about 3,000 ]s away in the ] ].<ref name="NYT-20240308">{{cite news |last=Andrews |first=Robin George |title=The Night Sky Will Soon Get 'a New Star.' Here's How to See It. - A nova named T Coronae Borealis lit up the night about 80 years ago, and astronomers say it's expected to put on another show in the coming months. |url=https://www.nytimes.com/article/nova-new-star-t-coronae-borealis.html |date=8 March 2024 |work=] |url-status=live |archiveurl=https://archive.today/20240308220630/https://www.nytimes.com/article/nova-new-star-t-coronae-borealis.html|archivedate=8 March 2024 |accessdate=9 March 2024 }}</ref> It was first discovered in outburst in 1866 by ],<ref name=pettit>{{cite journal|bibcode=1946PASP...58..153P|title=The Light-Curves of T Coronae Borealis|journal=Publications of the Astronomical Society of the Pacific|volume=58|pages=153|last1=Pettit|first1=Edison|year=1946|issue=341|doi=10.1086/125797|doi-access=free}}</ref> though it had been observed earlier as a 10th magnitude star.<ref name=barnard>{{cite journal|bibcode=1907ApJ....25..279B|title=Nova T Coronae of 1866|journal=Astrophysical Journal|volume=25|pages=279|last1=Barnard|first1=E. E.|year=1907|doi=10.1086/141446}}</ref> It may have been observed in 1217 and in 1787 as well.<ref>{{Cite journal |last=Schaefer |first=Bradley E. |date=16 November 2023 |title=The recurrent nova T CrB had prior eruptions observed near December 1787 and October 1217 AD |journal=Journal for the History of Astronomy |language=en |volume=54 |issue=4 |pages=436–455 |doi=10.1177/00218286231200492 |issn=0021-8286|arxiv=2308.13668 |bibcode=2023JHA....54..436S }}</ref><ref>{{Cite web |last=Thompson |first=Joanna |date=September 15, 2023 |title=Evidence of mysterious 'recurring nova' that could reappear in 2024 found in medieval manuscript from 1217 |url=https://www.livescience.com/space/astronomy/evidence-of-mysterious-recurring-nova-that-could-reappear-in-2024-found-in-medieval-manuscript-from-1217 |access-date=2024-03-21 |publisher=Live Science}}</ref>


==Description== ==Description==
] of T&nbsp;Coronae Borealis during the time surrounding its 1946 eruption, plotted from ] data]] ] of T&nbsp;Coronae Borealis during the time surrounding its 1946 eruption, plotted from ] data]]
T CrB normally has a ] of about 10, which is near the limit of typical binoculars. Outbursts have been seen twice, reaching magnitude 2.0 on May 12, 1866 and magnitude 3.0 on February 9, 1946,<ref name=Sanford1949/> although a more recent paper shows the 1866 outburst with a possible peak range of magnitude 2.5&nbsp;±&nbsp;0.5.<ref name=Schaefer2009/> Even when at peak magnitude of 2.5, this ] is dimmer than about 120 stars in the night sky.<ref name="SIMBAD-mag2.5">{{cite web |title=Vmag<2.5 |publisher=SIMBAD Astronomical Database |url=http://simbad.u-strasbg.fr/simbad/sim-sam?Criteria=Vmag%3C2.5 |accessdate=2010-06-25}}</ref> It is sometimes nicknamed the ''Blaze Star''.<ref>, 34. Unusual Stellar Spectra III: two emission-line stars</ref> T CrB normally has a ] of about 10, which is near the limit of typical binoculars. Well documented outbursts have been seen twice, reaching magnitude 2.0 on May 12, 1866 and magnitude 3.0 on February 9, 1946,<ref name=Sanford1949/> though a more recent paper shows the 1866 outburst with a possible peak range of magnitude 2.5&nbsp;±&nbsp;0.5.<ref name=Schaefer2009/> Even when at peak magnitude of 2.5, this ] is dimmer than about 120 stars in the night sky.<ref name="SIMBAD-mag2.5">{{cite web |title=Vmag<2.5 |publisher=SIMBAD Astronomical Database |url=http://simbad.u-strasbg.fr/simbad/sim-sam?Criteria=Vmag%3C2.5 |accessdate=2010-06-25}}</ref> It is sometimes nicknamed the ''Blaze Star''.<ref>{{cite journal |last1=Proctor |first1=Mary |date=June 1897 |title=Heavens for June |url=https://ui.adsabs.harvard.edu/abs/1897PA......5...97P/abstract |journal=Popular Astronomy |volume=5 |issue= |pages=104–105 |bibcode=1897PA......5...97P |access-date=2 July 2024}}</ref>


⚫ ]T CrB is a ] containing a large cool component and a smaller hot component. The cool component is a ] that transfers material to the hot component.<ref name=Kraft1958/> The hot component is a ] surrounded by an ], all hidden inside a dense cloud of material from the red giant. When the system is quiescent, the red giant dominates the visible light output and the system appears as an ] giant. The hot component contributes some emission and dominates the ] output. During outbursts, the transfer of material to the hot component increases greatly, the hot component expands, and the luminosity of the system increases.<ref name=linford/><ref name=stanishev/><ref name=ilkiewicz/><ref name=luna/>
In March 2024, B. E. Schaefer of Louisiana State University, Baton Rouge, reported the discovery of an apparent long-lost nova eruption of T CrB at visual magnitude somewhat brighter than +2, based on the eyewitness report of Burchard, Abbot of the Ursberg Abbey (near Augsberg, Germany), in the autumn of the year 1217.  This record appears in Latin in the Ursperger Chronicle, a medieval monastic annal written in the year 1225, and the nova was one of the two most important events of the year.


⚫ ] T CrB from 1 Jan 2008 to 17 Nov 2010, showing ]. Up is brighter and down is fainter. Day numbers are ].]]
Schaefer further reported his discovery of an eruption at visual magnitude somewhat brighter than 7.8, based on unpublished letters and catalogs of the English astronomer Rev. Francis Wollaston (F.R.S., Chislehurst, England).  Wollaston first mentioned the star in a letter to Sir William Herschel, dated 1787 Dec. 28.
⚫ The two components of the system orbit each other about every 228 days. The orbit is almost circular and is inclined at an angle of 67°. The stars are separated by {{val|0.54|ul=AU}}.<ref name=linford/>


⚫ ==2016–present activity==
⚫ T CrB is a ] containing a large cool component and a smaller hot component. The cool component is a ] which is transferring material to the hot component. The hot component is a ] surrounded by an ], all hidden inside a dense cloud of material from the red giant. When the system is quiescent, the red giant dominates the visible light output and the system appears as an ] giant. The hot component contributes some emission and dominates the ] output. During outbursts, the transfer of material to the hot component increases greatly, the hot component expands, and the luminosity of the system increases.<ref name=linford/><ref name=stanishev/><ref name=ilkiewicz/><ref name=luna/>
⚫ On 20 April 2016, the '']'' website reported a sustained brightening since February 2015 from magnitude 10.5 to about 9.2. A similar event was reported in 1938, followed by another outburst in 1946.<ref name=sandt>{{cite web|url=http://www.skyandtelescope.com/observing/whats-up-with-t-crb04202016|publisher=Sky & Telescope website|title=Is T CrB About to Blow its Top?|date=20 April 2016|accessdate=2017-08-06}}</ref> By June 2018, the star had dimmed slightly but still remained at an unusually high level of activity. By mid-2023, it faded by 0.35 magnitude; the lowest brightness seen since 2016.<ref>{{cite web |last1=Schaefer |first1=B.E. |last2=Kloppenborg |first2=B. |last3=Waagen |first3=E.O. |title=Announcing T CrB pre-eruption dip |url=https://www.aavso.org/news/t-crb-pre-eruption-dip |website=AAVSO |publisher=American Association of Variable Star Observers |access-date=18 January 2024}}</ref> A similar dimming occurred in the year before the 1946 outburst,<ref>{{cite web |last1=Todd |first1=Ian |title=T Coronae Borealis nova event guide and how to prepare |url=https://www.skyatnightmagazine.com/space-science/t-coronae-borealis-nova |website=Sky at Night Magazine |publisher=BBC |access-date=18 March 2024}}</ref> indicating an eruption before September 2024.<ref>{{Cite web |date=2024-06-06 |title=NASA, Global Astronomers Await Rare Nova Explosion - NASA |url=https://www.nasa.gov/centers-and-facilities/marshall/nasa-global-astronomers-await-rare-nova-explosion/ |access-date=2024-07-23 |language=en-US}}</ref> As of December 2024, such a nova has not yet been observed, although it is believed to be imminent.<ref>{{cite magazine |last1=Pearson |first1=Ezzy |last2=Lintott |first2=Chris |date=August 20, 2024 |title=T Coronae Borealis nova could become a 'new star' in the sky any day now, and will be as bright as the North Star |url=https://www.skyatnightmagazine.com/space-science/t-coronae-borealis-nova |magazine=BBC Sky at Night |location= |publisher=Our Media |access-date=3 September 2024}}</ref>


Predictions of the next nova:
⚫ ] T CrB from 1 Jan 2008 to 17 Nov 2010, showing the pulsations of the ] primary. Up is brighter and down is fainter. Day numbers are ].]]
⚫ The two components of the system orbit each other every 228 days. The orbit is almost circular and is inclined at an angle of 67°. The stars are separated by {{val|0.54|ul=AU}}.<ref name=linford/>

⚫ ==2016–present activity==
⚫ On 20 April 2016, the '']'' website reported a sustained brightening since February 2015 from magnitude 10.5 to about 9.2. A similar event was reported in 1938, followed by another outburst in 1946.<ref name=sandt>{{cite web|url=http://www.skyandtelescope.com/observing/whats-up-with-t-crb04202016|publisher=Sky & Telescope website|title=Is T CrB About to Blow its Top?|date=20 April 2016|accessdate=2017-08-06}}</ref> By June 2018, the star had dimmed slightly but still remained at an unusually high level of activity. In March or April 2023, it dimmed to magnitude 12.3.<ref>{{cite web |last1=Schaefer |first1=B.E. |last2=Kloppenborg |first2=B. |last3=Waagen |first3=E.O. |title=Announcing T CrB pre-eruption dip |url=https://www.aavso.org/news/t-crb-pre-eruption-dip |website=AAVSO |publisher=American Association of Variable Star Observers |access-date=18 January 2024}}</ref> A similar dimming occurred in the year before the 1946 outburst, indicating that it will likely erupt between March and September 2024.<ref>{{cite web |last1=Todd |first1=Ian |title=T Coronae Borealis nova event guide and how to prepare |url=https://www.skyatnightmagazine.com/space-science/t-coronae-borealis-nova |website=Sky at Night Magazine |publisher=BBC |access-date=18 March 2024}}</ref>


* 2026-2027 (made in 1946 either by N.F.H.Knight or W.M. Lindley)<ref>{{Cite journal |last=Shears |first=J. H. |date=2024-06-01 |title=An Independent Discovery of the 1946 Eruption of the Recurrent Nova T Coronae Borealis and an Early Prediction of a Future Outburst |journal=Research Notes of the American Astronomical Society |volume=8 |issue=6 |pages=157 |bibcode=2024RNAAS...8..157S |doi=10.3847/2515-5172/ad566b |doi-access=free |issn=2515-5172}}</ref>
* Mid February 2024 to end September 2026 (made in March 2023)<ref>{{Cite journal |last=Schaefer |first=Bradley E. |date=2023-09-01 |title=The B & V light curves for recurrent nova T CrB from 1842-2022, the unique pre- and post-eruption high-states, the complex period changes, and the upcoming eruption in 2025.5 ± 1.3 |journal=Monthly Notices of the Royal Astronomical Society |volume=524 |issue=2 |pages=3146–3165 |arxiv=2303.04933 |bibcode=2023MNRAS.524.3146S |doi=10.1093/mnras/stad735 |doi-access=free |issn=0035-8711}}</ref>
* Beginning January 2024 to mid August 2024 (made in June 2023)<ref>{{Cite journal |last1=Schaefer |first1=Bradley E. |last2=Kloppenborg |first2=Brian |last3=Waagen |first3=Elizabeth O. |last4=Observers |first4=The Aavso |date=2023-06-01 |title=Recurrent nova T CrB has just started its Pre-eruption Dip in March/April 2023, so the eruption should occur around 2024.4 +- 0.3 |url=https://ui.adsabs.harvard.edu/abs/2023ATel16107....1S/abstract |journal=The Astronomer's Telegram |volume=16107 |pages=1 |bibcode=2023ATel16107....1S}}</ref>
* January 2024 (made in August 2023)<ref>{{Cite journal |last1=Maslennikova |first1=N. A. |last2=Tatarnikov |first2=A. M. |last3=Tatarnikova |first3=A. A. |last4=Dodin |first4=A. V. |last5=Shenavrin |first5=V. I. |last6=Burlak |first6=M. A. |last7=Zheltoukhov |first7=S. G. |last8=Strakhov |first8=I. A. |date=2023-10-01 |title=Recurrent Symbiotic Nova T Coronae Borealis before Outburst |url=https://ui.adsabs.harvard.edu/abs/2023AstL...49..501M/abstract |journal=Astronomy Letters |volume=49 |issue=9 |pages=501–515 |arxiv=2308.10011 |bibcode=2023AstL...49..501M |doi=10.1134/S1063773723090037 |issn=1063-7737}}</ref>
* End of October 2024 (made in June 2024)<ref>{{Cite journal |last1=Toalá |first1=Jesús A. |last2=González-Martín |first2=Omaira |last3=Sacchi |first3=Andrea |last4=Vasquez-Torres |first4=Diego A. |date=2024-08-01 |title=The X-ray rise and fall of the symbiotic recurrent nova system T CrB |journal=Monthly Notices of the Royal Astronomical Society |volume=532 |issue=2 |pages=1421–1433 |arxiv=2405.08980 |bibcode=2024MNRAS.532.1421T |doi=10.1093/mnras/stae1579 |doi-access=free |issn=0035-8711}}</ref>
* Around 27 March 2025, 10 November 2025, 25 June 2026 or 8 February 2027 (made in October 2024)<ref>{{Cite journal |last=Schneider |first=Jean |date=October 2024 |title=When will the Next T CrB Eruption Occur? |journal=Research Notes of the AAS |language=en |volume=8 |issue=10 |pages=272 |doi=10.3847/2515-5172/ad8bba |doi-access=free |bibcode=2024RNAAS...8..272S |issn=2515-5172}}</ref>
{{Clear|left}} {{Clear|left}}


==References== ==References==
{{Reflist|refs= {{Reflist|30em|refs=

⚫ <ref name=GaiaDR3>{{Cite Gaia DR3|1220110705972528512}}</ref>


<ref name=stanishev>{{cite journal|bibcode=2004A&A...415..609S|title=Hα variability of the recurrent nova T Coronae Borealis|journal=Astronomy and Astrophysics|volume=415|issue=2|pages=609–616|last1=Stanishev|first1=V.|last2=Zamanov|first2=R.|last3=Tomov|first3=N.|last4=Marziani|first4=P.|year=2004|doi=10.1051/0004-6361:20034623|arxiv = astro-ph/0311309 |s2cid=3000175}}</ref> <ref name=stanishev>{{cite journal|bibcode=2004A&A...415..609S|title=Hα variability of the recurrent nova T Coronae Borealis|journal=Astronomy and Astrophysics|volume=415|issue=2|pages=609–616|last1=Stanishev|first1=V.|last2=Zamanov|first2=R.|last3=Tomov|first3=N.|last4=Marziani|first4=P.|year=2004|doi=10.1051/0004-6361:20034623|arxiv = astro-ph/0311309 |s2cid=3000175}}</ref>
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|bibcode = 2010ApJS..187..275S |s2cid=119294221 |bibcode = 2010ApJS..187..275S |s2cid=119294221
}}</ref> }}</ref>

<!-- <ref name=Schaefer2023>{{Cite journal|last=Schaefer |first=Bradley E.
|title=The B & V light curves for recurrent nova T CrB from 1842-2022, the unique pre- and post-eruption high-states, the complex period changes, and the upcoming eruption in 2025.5 ± 1.3
|journal=Monthly Notices of the Royal Astronomical Society
|volume=524
|issue=2
|pages=3146–3165
|year=2023
|arxiv=2303.04933|doi=10.1093/mnras/stad735
|bibcode=2023MNRAS.524.3146S
}}</ref> -->


<ref name=Sanford1949>{{cite journal <ref name=Sanford1949>{{cite journal
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|doi=10.1086/145106 |doi=10.1086/145106
|bibcode=1949ApJ...109...81S|doi-access=free |bibcode=1949ApJ...109...81S|doi-access=free
}}</ref>

⚫ <ref name=Kraft1958>{{cite journal
|last=Kraft |first=Robert P.
|title=The Binary System Nova T Coronae Borealis.
|journal=Astrophysical Journal
|volume=127 |pages=625 |year=1958
|doi=10.1086/146495
|bibcode=1958ApJ...127..625K|doi-access=free
}}</ref> }}</ref>


<ref name=gcvs>{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S|volume=1|display-authors=etal|last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}</ref> <ref name=gcvs>{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S|volume=1|display-authors=etal|last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}</ref>

⚫ <ref name=dr1>{{cite journal
| title=Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties
| display-authors=1 | author1=Gaia Collaboration
| last2=Brown | first2=A. G. A. | last3=Vallenari | first3=A.
| last4=Prusti | first4=T. | last5=de Bruijne | first5=J. H. J.
| last6=Mignard | first6=F. | last7=Drimmel | first7=R.
| journal=Astronomy & Astrophysics | volume=595 | id=A2 | pages=23 | date=November 2016
| doi=10.1051/0004-6361/201629512 | bibcode=2016A&A...595A...2G |arxiv = 1609.04172 | s2cid=1828208 }}</ref>


<ref name=shenavrin>{{cite journal|bibcode=2011ARep...55...31S|title=Search for and study of hot circumstellar dust envelopes|journal=Astronomy Reports|volume=55|pages=31–81|last1=Shenavrin|first1=V. I.|last2=Taranova|first2=O. G.|last3=Nadzhip|first3=A. E.|year=2011|issue=1|doi=10.1134/S1063772911010070|s2cid=122700080}}</ref> <ref name=shenavrin>{{cite journal|bibcode=2011ARep...55...31S|title=Search for and study of hot circumstellar dust envelopes|journal=Astronomy Reports|volume=55|pages=31–81|last1=Shenavrin|first1=V. I.|last2=Taranova|first2=O. G.|last3=Nadzhip|first3=A. E.|year=2011|issue=1|doi=10.1134/S1063772911010070|s2cid=122700080}}</ref>
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<ref name=orbit>{{cite journal|bibcode=2004A&A...424..727P|title=SB9: The ninth catalogue of spectroscopic binary orbits|journal=Astronomy and Astrophysics|volume=424|issue=2|pages=727–732|last1=Pourbaix|first1=D.|last2=Tokovinin|first2=A. A.|last3=Batten|first3=A. H.|last4=Fekel|first4=F. C.|last5=Hartkopf|first5=W. I.|last6=Levato|first6=H.|last7=Morrell|first7=N. I.|author-link7=Nidia Morrell|last8=Torres|first8=G.|last9=Udry|first9=S.|year=2004|doi=10.1051/0004-6361:20041213|arxiv = astro-ph/0406573 |s2cid=119387088}}</ref> <ref name=orbit>{{cite journal|bibcode=2004A&A...424..727P|title=SB9: The ninth catalogue of spectroscopic binary orbits|journal=Astronomy and Astrophysics|volume=424|issue=2|pages=727–732|last1=Pourbaix|first1=D.|last2=Tokovinin|first2=A. A.|last3=Batten|first3=A. H.|last4=Fekel|first4=F. C.|last5=Hartkopf|first5=W. I.|last6=Levato|first6=H.|last7=Morrell|first7=N. I.|author-link7=Nidia Morrell|last8=Torres|first8=G.|last9=Udry|first9=S.|year=2004|doi=10.1051/0004-6361:20041213|arxiv = astro-ph/0406573 |s2cid=119387088}}</ref>


<ref name=ilkiewicz>{{cite journal|bibcode=2016MNRAS.462.2695I|arxiv=1607.06804|title=Active phases and flickering of a symbiotic recurrent nova T CrB|journal=Monthly Notices of the Royal Astronomical Society|volume=462|issue=3|pages=2695|last1=Iłkiewicz|first1=Krystian|last2=Mikołajewska|first2=Joanna|last3=Stoyanov|first3=Kiril|last4=Manousakis|first4=Antonios|last5=Miszalski|first5=Brent|year=2016|doi=10.1093/mnras/stw1837|s2cid=119104759}}</ref> <ref name=ilkiewicz>{{cite journal|bibcode=2016MNRAS.462.2695I|arxiv=1607.06804|title=Active phases and flickering of a symbiotic recurrent nova T CrB|journal=Monthly Notices of the Royal Astronomical Society|volume=462|issue=3|pages=2695|last1=Iłkiewicz|first1=Krystian|last2=Mikołajewska|first2=Joanna|last3=Stoyanov|first3=Kiril|last4=Manousakis|first4=Antonios|last5=Miszalski|first5=Brent|year=2016|doi=10.1093/mnras/stw1837|doi-access=free |s2cid=119104759}}</ref>


<ref name=luna>{{cite journal|bibcode=2018A&A...619A..61L|arxiv=1807.01304|title=Dramatic change in the boundary layer in the symbiotic recurrent nova T Coronae Borealis|journal=Astronomy and Astrophysics|volume=619|issue=1|pages=61|last1=Luna|first1=GJM|last2=Mukai|first2=K.|last3=Sokoloski|first3=J. L.|last4=Nelson|first4=T.|last5=Kuin|first5=P.|last6=Segreto|first6=A.|last7=Cusumano|first7=G.|last8=Jaque Arancibia|first8=M.|last9=Nuñez|first9=N. E.|year=2018|doi=10.1051/0004-6361/201833747|s2cid=119078482}}</ref> <ref name=luna>{{cite journal|bibcode=2018A&A...619A..61L|arxiv=1807.01304|title=Dramatic change in the boundary layer in the symbiotic recurrent nova T Coronae Borealis|journal=Astronomy and Astrophysics|volume=619|issue=1|pages=61|last1=Luna|first1=GJM|last2=Mukai|first2=K.|last3=Sokoloski|first3=J. L.|last4=Nelson|first4=T.|last5=Kuin|first5=P.|last6=Segreto|first6=A.|last7=Cusumano|first7=G.|last8=Jaque Arancibia|first8=M.|last9=Nuñez|first9=N. E.|year=2018|doi=10.1051/0004-6361/201833747|s2cid=119078482}}</ref>



<ref name=wallerstein>{{cite journal|bibcode=2008PASP..120..492W|title=The Metallicity and Lithium Abundances of the Recurring Novae T CrB and RS Oph|journal=Publications of the Astronomical Society of the Pacific|volume=120|issue=867|pages=492|last1=Wallerstein|first1=George|last2=Harrison|first2=Tanya|last3=Munari|first3=Ulisse|last4=Vanture|first4=Andrew|year=2008|doi=10.1086/587965|s2cid=106406607 |doi-access=free}}</ref> <ref name=wallerstein>{{cite journal|bibcode=2008PASP..120..492W|title=The Metallicity and Lithium Abundances of the Recurring Novae T CrB and RS Oph|journal=Publications of the Astronomical Society of the Pacific|volume=120|issue=867|pages=492|last1=Wallerstein|first1=George|last2=Harrison|first2=Tanya|last3=Munari|first3=Ulisse|last4=Vanture|first4=Andrew|year=2008|doi=10.1086/587965|s2cid=106406607 |doi-access=free}}</ref>
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<ref name=schaefer>{{cite journal |bibcode=2009ApJ...697..721S |title=Orbital Periods for Three Recurrent Novae |journal=The Astrophysical Journal |volume=697 |issue=1 |pages=721–729 |last1=Schaefer |first1=Bradley E. |year=2009 |arxiv=0903.1349 |doi=10.1088/0004-637X/697/1/721 |s2cid=16087253 }}</ref> <ref name=schaefer>{{cite journal |bibcode=2009ApJ...697..721S |title=Orbital Periods for Three Recurrent Novae |journal=The Astrophysical Journal |volume=697 |issue=1 |pages=721–729 |last1=Schaefer |first1=Bradley E. |year=2009 |arxiv=0903.1349 |doi=10.1088/0004-637X/697/1/721 |s2cid=16087253 }}</ref>

⚫ <ref name=dr2>{{cite DR2|1220110705972528512}}</ref>


}} }}
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==Further reading== ==Further reading==
*{{cite journal | last = Wallerstein | first = George |author2=Tanya Harrison |author3=Ulisse Munari |author4=Andrew Vanture | date = 11 May 2008 | title = The Metallicity and Lithium Abundances of the Recurring Novae T CrB and RS Oph | journal = ] | volume = 120 | issue = 867 | pages = 492–497 | doi = 10.1086/587965 | bibcode=2008PASP..120..492W| s2cid = 106406607 | doi-access = free }} *{{cite journal | last = Wallerstein | first = George |author2=Tanya Harrison |author3=Ulisse Munari |author4=Andrew Vanture | date = 11 May 2008 | title = The Metallicity and Lithium Abundances of the Recurring Novae T CrB and RS Oph | journal = ] | volume = 120 | issue = 867 | pages = 492–497 | doi = 10.1086/587965 | bibcode=2008PASP..120..492W| s2cid = 106406607 | doi-access = free }}
* {{Webarchive|url=https://web.archive.org/web/20120406100800/http://www.skyandtelescope.com/observing/objects/variablestars/3310256.html |date=2012-04-06 }} at Sky & Telescope * at Sky & Telescope {{Webarchive|url=https://web.archive.org/web/20120406100800/http://www.skyandtelescope.com/observing/objects/variablestars/3310256.html |date=2012-04-06 }}


==External links== ==External links==
* http://www.daviddarling.info/encyclopedia/B/Blaze_Star.html * , www.daviddarling.info
* AAVSO: (get recent magnitude estimates for T CrB) * AAVSO: (get recent magnitude estimates for T CrB)


{{2024 in space}}
{{Stars of Corona Borealis}} {{Stars of Corona Borealis}}


Latest revision as of 10:24, 12 December 2024

Recurrent nova in the constellation Corona BorealisNot to be confused with Tau Coronae Borealis.
T Coronae Borealis
Location of T Coronae Borealis (circled in red)
Observation data
Epoch J2000      Equinox J2000
Constellation Corona Borealis
Right ascension 15 59 30.1622
Declination +25° 55′ 12.613″
Apparent magnitude (V) 2.0–10.8
Characteristics
Evolutionary stage Red giant + white dwarf
Spectral type M3III+p
Variable type recurrent nova
Astrometry
Radial velocity (Rv)−27.79 km/s
Proper motion (μ) RA: −4.461 mas/yr
Dec.: 12.016 mas/yr
Parallax (π)1.0920 ± 0.0275 mas
Distance2,990 ± 80 ly
(920 ± 20 pc)
Orbit
Period (P)227.55 d
Semi-major axis (a)0.54 AU
Eccentricity (e)0.0
Inclination (i)67°
Details
Red giant
Mass1.12 M☉
Radius75 R☉
Luminosity655 L☉
Surface gravity (log g)2.0 cgs
Temperature3,600 K
White dwarf
Mass1.37 M☉
Luminosity~100 L☉
Other designations
BD+26° 2765, HD 143454, HIP 78322, HR 5958, SAO 84129, 2MASS J15593015+2555126, T Cor Bor
Database references
SIMBADdata

T Coronae Borealis (T CrB), nicknamed the Blaze Star, is a binary star and a recurrent nova about 3,000 light-years away in the constellation Corona Borealis. It was first discovered in outburst in 1866 by John Birmingham, though it had been observed earlier as a 10th magnitude star. It may have been observed in 1217 and in 1787 as well.

Description

The light curve of T Coronae Borealis during the time surrounding its 1946 eruption, plotted from AAVSO data

T CrB normally has a magnitude of about 10, which is near the limit of typical binoculars. Well documented outbursts have been seen twice, reaching magnitude 2.0 on May 12, 1866 and magnitude 3.0 on February 9, 1946, though a more recent paper shows the 1866 outburst with a possible peak range of magnitude 2.5 ± 0.5. Even when at peak magnitude of 2.5, this recurrent nova is dimmer than about 120 stars in the night sky. It is sometimes nicknamed the Blaze Star.

T Coronae Borealis based on a description given by Kraft using the updated mass ratio given by Stanishev

T CrB is a binary system containing a large cool component and a smaller hot component. The cool component is a red giant that transfers material to the hot component. The hot component is a white dwarf surrounded by an accretion disc, all hidden inside a dense cloud of material from the red giant. When the system is quiescent, the red giant dominates the visible light output and the system appears as an M3 giant. The hot component contributes some emission and dominates the ultraviolet output. During outbursts, the transfer of material to the hot component increases greatly, the hot component expands, and the luminosity of the system increases.

AAVSO light curve of recurrent nova T CrB from 1 Jan 2008 to 17 Nov 2010, showing rotating ellipsoidal variability. Up is brighter and down is fainter. Day numbers are Julian day.

The two components of the system orbit each other about every 228 days. The orbit is almost circular and is inclined at an angle of 67°. The stars are separated by 0.54 AU.

2016–present activity

On 20 April 2016, the Sky & Telescope website reported a sustained brightening since February 2015 from magnitude 10.5 to about 9.2. A similar event was reported in 1938, followed by another outburst in 1946. By June 2018, the star had dimmed slightly but still remained at an unusually high level of activity. By mid-2023, it faded by 0.35 magnitude; the lowest brightness seen since 2016. A similar dimming occurred in the year before the 1946 outburst, indicating an eruption before September 2024. As of December 2024, such a nova has not yet been observed, although it is believed to be imminent.

Predictions of the next nova:

  • 2026-2027 (made in 1946 either by N.F.H.Knight or W.M. Lindley)
  • Mid February 2024 to end September 2026 (made in March 2023)
  • Beginning January 2024 to mid August 2024 (made in June 2023)
  • January 2024 (made in August 2023)
  • End of October 2024 (made in June 2024)
  • Around 27 March 2025, 10 November 2025, 25 June 2026 or 8 February 2027 (made in October 2024)

References

  1. ^ Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. Shenavrin, V. I.; Taranova, O. G.; Nadzhip, A. E. (2011). "Search for and study of hot circumstellar dust envelopes". Astronomy Reports. 55 (1): 31–81. Bibcode:2011ARep...55...31S. doi:10.1134/S1063772911010070. S2CID 122700080.
  4. Pourbaix, D.; Tokovinin, A. A.; Batten, A. H.; Fekel, F. C.; Hartkopf, W. I.; Levato, H.; Morrell, N. I.; Torres, G.; Udry, S. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727–732. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. S2CID 119387088.
  5. ^ Fekel, Francis C.; Joyce, Richard R.; Hinkle, Kenneth H.; Skrutskie, Michael F. (2000). "Infrared Spectroscopy of Symbiotic Stars. I. Orbits for Well-Known S-Type Systems". The Astronomical Journal. 119 (3): 1375. Bibcode:2000AJ....119.1375F. doi:10.1086/301260.
  6. ^ Linford, Justin D.; Chomiuk, Laura; Sokoloski, Jennifer L.; Weston, Jennifer H. S.; Van Der Horst, Alexander J.; Mukai, Koji; Barrett, Paul; Mioduszewski, Amy J.; Rupen, Michael (2019). "T CRB: Radio Observations during the 2016-2017 "Super-active" State". The Astrophysical Journal. 884 (1): 8. arXiv:1909.13858. Bibcode:2019ApJ...884....8L. doi:10.3847/1538-4357/ab3c62. S2CID 203593955.
  7. ^ Stanishev, V.; Zamanov, R.; Tomov, N.; Marziani, P. (2004). "Hα variability of the recurrent nova T Coronae Borealis". Astronomy and Astrophysics. 415 (2): 609–616. arXiv:astro-ph/0311309. Bibcode:2004A&A...415..609S. doi:10.1051/0004-6361:20034623. S2CID 3000175.
  8. Schaefer, Bradley E. (2009). "Orbital Periods for Three Recurrent Novae". The Astrophysical Journal. 697 (1): 721–729. arXiv:0903.1349. Bibcode:2009ApJ...697..721S. doi:10.1088/0004-637X/697/1/721. S2CID 16087253.
  9. ^ Wallerstein, George; Harrison, Tanya; Munari, Ulisse; Vanture, Andrew (2008). "The Metallicity and Lithium Abundances of the Recurring Novae T CrB and RS Oph". Publications of the Astronomical Society of the Pacific. 120 (867): 492. Bibcode:2008PASP..120..492W. doi:10.1086/587965. S2CID 106406607.
  10. Starrfield, Sumner; Bose, Maitrayee; Woodward, Charles E.; Perron, Isabelle; Shaw, Gargi; Evans, Aneurin; Iliadis, Christian; Hix, W. Raphael (2024-06-01). "The evolution leading to a thermonuclear runaway". Bulletin of the American Astronomical Society. 56 (7): 132.01. Bibcode:2024AAS...24413201S.
  11. Andrews, Robin George (8 March 2024). "The Night Sky Will Soon Get 'a New Star.' Here's How to See It. - A nova named T Coronae Borealis lit up the night about 80 years ago, and astronomers say it's expected to put on another show in the coming months". The New York Times. Archived from the original on 8 March 2024. Retrieved 9 March 2024.
  12. Pettit, Edison (1946). "The Light-Curves of T Coronae Borealis". Publications of the Astronomical Society of the Pacific. 58 (341): 153. Bibcode:1946PASP...58..153P. doi:10.1086/125797.
  13. Barnard, E. E. (1907). "Nova T Coronae of 1866". Astrophysical Journal. 25: 279. Bibcode:1907ApJ....25..279B. doi:10.1086/141446.
  14. Schaefer, Bradley E. (16 November 2023). "The recurrent nova T CrB had prior eruptions observed near December 1787 and October 1217 AD". Journal for the History of Astronomy. 54 (4): 436–455. arXiv:2308.13668. Bibcode:2023JHA....54..436S. doi:10.1177/00218286231200492. ISSN 0021-8286.
  15. Thompson, Joanna (September 15, 2023). "Evidence of mysterious 'recurring nova' that could reappear in 2024 found in medieval manuscript from 1217". Live Science. Retrieved 2024-03-21.
  16. Sanford, Roscoe F. (1949). "High-Dispersion Spectrograms of T Coronae Borealis". Astrophysical Journal. 109: 81. Bibcode:1949ApJ...109...81S. doi:10.1086/145106.
  17. Schaefer, Bradley E. (2010). "Comprehensive Photometric Histories of All Known Galactic Recurrent Novae". The Astrophysical Journal Supplement Series. 187 (2): 275–373. arXiv:0912.4426. Bibcode:2010ApJS..187..275S. doi:10.1088/0067-0049/187/2/275. S2CID 119294221.
  18. "Vmag<2.5". SIMBAD Astronomical Database. Retrieved 2010-06-25.
  19. Proctor, Mary (June 1897). "Heavens for June". Popular Astronomy. 5: 104–105. Bibcode:1897PA......5...97P. Retrieved 2 July 2024.
  20. ^ Kraft, Robert P. (1958). "The Binary System Nova T Coronae Borealis". Astrophysical Journal. 127: 625. Bibcode:1958ApJ...127..625K. doi:10.1086/146495.
  21. Iłkiewicz, Krystian; Mikołajewska, Joanna; Stoyanov, Kiril; Manousakis, Antonios; Miszalski, Brent (2016). "Active phases and flickering of a symbiotic recurrent nova T CrB". Monthly Notices of the Royal Astronomical Society. 462 (3): 2695. arXiv:1607.06804. Bibcode:2016MNRAS.462.2695I. doi:10.1093/mnras/stw1837. S2CID 119104759.
  22. Luna, GJM; Mukai, K.; Sokoloski, J. L.; Nelson, T.; Kuin, P.; Segreto, A.; Cusumano, G.; Jaque Arancibia, M.; Nuñez, N. E. (2018). "Dramatic change in the boundary layer in the symbiotic recurrent nova T Coronae Borealis". Astronomy and Astrophysics. 619 (1): 61. arXiv:1807.01304. Bibcode:2018A&A...619A..61L. doi:10.1051/0004-6361/201833747. S2CID 119078482.
  23. "Is T CrB About to Blow its Top?". Sky & Telescope website. 20 April 2016. Retrieved 2017-08-06.
  24. Schaefer, B.E.; Kloppenborg, B.; Waagen, E.O. "Announcing T CrB pre-eruption dip". AAVSO. American Association of Variable Star Observers. Retrieved 18 January 2024.
  25. Todd, Ian. "T Coronae Borealis nova event guide and how to prepare". Sky at Night Magazine. BBC. Retrieved 18 March 2024.
  26. "NASA, Global Astronomers Await Rare Nova Explosion - NASA". 2024-06-06. Retrieved 2024-07-23.
  27. Pearson, Ezzy; Lintott, Chris (August 20, 2024). "T Coronae Borealis nova could become a 'new star' in the sky any day now, and will be as bright as the North Star". BBC Sky at Night. Our Media. Retrieved 3 September 2024.
  28. Shears, J. H. (2024-06-01). "An Independent Discovery of the 1946 Eruption of the Recurrent Nova T Coronae Borealis and an Early Prediction of a Future Outburst". Research Notes of the American Astronomical Society. 8 (6): 157. Bibcode:2024RNAAS...8..157S. doi:10.3847/2515-5172/ad566b. ISSN 2515-5172.
  29. Schaefer, Bradley E. (2023-09-01). "The B & V light curves for recurrent nova T CrB from 1842-2022, the unique pre- and post-eruption high-states, the complex period changes, and the upcoming eruption in 2025.5 ± 1.3". Monthly Notices of the Royal Astronomical Society. 524 (2): 3146–3165. arXiv:2303.04933. Bibcode:2023MNRAS.524.3146S. doi:10.1093/mnras/stad735. ISSN 0035-8711.
  30. Schaefer, Bradley E.; Kloppenborg, Brian; Waagen, Elizabeth O.; Observers, The Aavso (2023-06-01). "Recurrent nova T CrB has just started its Pre-eruption Dip in March/April 2023, so the eruption should occur around 2024.4 +- 0.3". The Astronomer's Telegram. 16107: 1. Bibcode:2023ATel16107....1S.
  31. Maslennikova, N. A.; Tatarnikov, A. M.; Tatarnikova, A. A.; Dodin, A. V.; Shenavrin, V. I.; Burlak, M. A.; Zheltoukhov, S. G.; Strakhov, I. A. (2023-10-01). "Recurrent Symbiotic Nova T Coronae Borealis before Outburst". Astronomy Letters. 49 (9): 501–515. arXiv:2308.10011. Bibcode:2023AstL...49..501M. doi:10.1134/S1063773723090037. ISSN 1063-7737.
  32. Toalá, Jesús A.; González-Martín, Omaira; Sacchi, Andrea; Vasquez-Torres, Diego A. (2024-08-01). "The X-ray rise and fall of the symbiotic recurrent nova system T CrB". Monthly Notices of the Royal Astronomical Society. 532 (2): 1421–1433. arXiv:2405.08980. Bibcode:2024MNRAS.532.1421T. doi:10.1093/mnras/stae1579. ISSN 0035-8711.
  33. Schneider, Jean (October 2024). "When will the Next T CrB Eruption Occur?". Research Notes of the AAS. 8 (10): 272. Bibcode:2024RNAAS...8..272S. doi:10.3847/2515-5172/ad8bba. ISSN 2515-5172.

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