Blaze Star - Revision history

IanRidpath: /* Occurance of the Name */ Typos

2026-02-18T08:48:53Z

Occurance of the Name: Typos

← Older revision		Revision as of 08:48, 18 February 2026
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	'''Note:''' We have no less than two data points (nova light curves) from the star whose eruption we are now expecting. One of these dates back to before the invention of electrical photometry (Potsdam, 1913), i.e., it is based solely on the estimates of experienced observers: a well-functioning method, but not using the same measurement method we use today. Contrary to everything taught in basic physics courses (or any laboratory course), we have no choice but to compare measurements that school physics teaches us are not comparable (common practice in astronomy).		'''Note:''' We have no less than two data points (nova light curves) from the star whose eruption we are now expecting. One of these dates back to before the invention of electrical photometry (Potsdam, 1913), i.e., it is based solely on the estimates of experienced observers: a well-functioning method, but not using the same measurement method we use today. Contrary to everything taught in basic physics courses (or any laboratory course), we have no choice but to compare measurements that school physics teaches us are not comparable (common practice in astronomy).

	=== ~~Occurance~~ of the Name ===		=== Occurrence of the Name ===
	The nickname has been around since the late 19th century, and it has propagated in astronomy literature significantly since then. WGSN found that the first recorded use of the name Blaze Star for T CrB was in a lecture by the British spectroscopist William Allen Miller at a meeting of the British Association in 1869, and published in the ''English Mechanic''. The name was popularized by R. A. Proctor (1872, see [https://books.google.de/books?id=bLJXAAAAYAAJ&pg=PA378&dq=Coronae+%22Blaze+star%22&hl=en&newbks=1&newbks_redir=0&sa=X&redir_esc=y#v=onepage&q=Coronae%20%22Blaze%20star%22&f=true GoogleBooks])<ref>Proctor, Richard A. (1872). The star depths. The Mechanics' Magazine, 96, 378-379.</ref> and later his daughter Mary Proctor (1897, see [https://articles.adsabs.harvard.edu/pdf/1897PA......5...97P on adsabs], p.104).		The nickname has been around since the late 19th century, and it has propagated in astronomy literature significantly since then. WGSN found that the first recorded use of the name Blaze Star for T CrB was in a lecture by the British spectroscopist William Allen Miller at a meeting of the British Association in 1869, and published in the ''English Mechanic''. The name was popularized by R. A. Proctor (1872, see [https://books.google.de/books?id=bLJXAAAAYAAJ&pg=PA378&dq=Coronae+%22Blaze+star%22&hl=en&newbks=1&newbks_redir=0&sa=X&redir_esc=y#v=onepage&q=Coronae%20%22Blaze%20star%22&f=true GoogleBooks])<ref>Proctor, Richard A. (1872). The star depths. The Mechanics' Magazine, 96, 378-379.</ref> and later his daughter Mary Proctor (1897, see [https://articles.adsabs.harvard.edu/pdf/1897PA......5...97P on adsabs], p.104).
	[[File:Blaze Star ProctorMary.png\|thumb\|Screenshot from [https://articles.adsabs.harvard.edu/pdf/1897PA......5...97P Mary Proctor's paper] (CC BY Ian Ridpath).]]		[[File:Blaze Star ProctorMary.png\|thumb\|Screenshot from [https://articles.adsabs.harvard.edu/pdf/1897PA......5...97P Mary Proctor's paper] (CC BY Ian Ridpath).]]
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	However, thename "Blaze Star" for the specific object in Corona Borealis is first found in the note in the [https://books.google.com/books?id=xj48AQAAMAAJ&pg=PA515 English Mechanic and Mirror Science in September 1869], displayed above.		However, thename "Blaze Star" for the specific object in Corona Borealis is first found in the note in the [https://books.google.com/books?id=xj48AQAAMAAJ&pg=PA515 English Mechanic and Mirror Science in September 1869], displayed above.

	=== ~~Expections~~ for next eruption ===		=== Expectations for next eruption ===
	Three of the other T CrB-class star systems erupt somewhat more frequently: every 20 to 30 years, so that what the press tells us about the impending eruption may not be entirely reliable. We suspect that during the outburst, the star will have approximately the brightness (3 to 2 mag) of the North Star or the main star of a constellation (alf CrB, [[Alphecca]]), because this was the case in both documented observations. Many (50%) recurrent novae always erupt with the same brightness – but the peak brightness can also vary (the other 50%). Therefore, it cannot be completely ruled out that the star T CrB will not be quite as bright as last time (e.g., only 4 mag or even only 6 mag) or that it will be even brighter (up to Arcturus brightness) during its upcoming outburst: We will only know for sure when we see it.		Three of the other T CrB-class star systems erupt somewhat more frequently: every 20 to 30 years, so that what the press tells us about the impending eruption may not be entirely reliable. We suspect that during the outburst, the star will have approximately the brightness (3 to 2 mag) of the North Star or the main star of a constellation (alf CrB, [[Alphecca]]), because this was the case in both documented observations. Many (50%) recurrent novae always erupt with the same brightness – but the peak brightness can also vary (the other 50%). Therefore, it cannot be completely ruled out that the star T CrB will not be quite as bright as last time (e.g., only 4 mag or even only 6 mag) or that it will be even brighter (up to Arcturus brightness) during its upcoming outburst: We will only know for sure when we see it.

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	*		*

	== ~~Reference~~ ==		== References ==
	* [[References\|References (general)]]		* [[References\|References (general)]]
	* Ian Ridpath's website ([http://www.ianridpath.com/startales/coronaborealis.html#blaze Star Tales, Corona Borealis] )		* Ian Ridpath's website ([http://www.ianridpath.com/startales/coronaborealis.html#blaze Star Tales, Corona Borealis] )

IanRidpath: Copyedit, better link

2026-02-18T08:46:51Z

Copyedit, better link

← Older revision		Revision as of 08:46, 18 February 2026
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	[[File:EnglishMechanicAndMirrorOfScience1869 content hi.jpg\|thumb\|screenshot of a page in the English Mechanic and Mirror Science, Sept 1869 - Here, the name "Blaze Star, 1866" is chosen as a headline]]		[[File:EnglishMechanicAndMirrorOfScience1869 content hi.jpg\|thumb\|screenshot of a page in the English Mechanic and Mirror Science, Sept 1869 - Here, the name "Blaze Star, 1866" is chosen as a headline]]
	[[File:TCrB bsc1990-768x485.jpg\|thumb\|The variable star T CrB is included in the Yale Bright Star Catalog (HR 5859), here depicted in a star chart in Hoffmann (2017).]]		[[File:TCrB bsc1990-768x485.jpg\|thumb\|The variable star T CrB is included in the Yale Bright Star Catalog (HR 5859), here depicted in a star chart in Hoffmann (2017).]]
	The name "Blaze Star" as a nickname for the eruptive variable T CrB ([https://simbad.cds.unistra.fr/simbad/sim-basic?Ident=T+CrB&submit=SIMBAD+search Simbad], [https://vsx.aavso.org/index.php?view=detail.top&oid=10602 VSX]) ~~ha sbeen~~ used since the 19th century. The symbiotic system in [[Corona Borealis]] consists of a red giant and a white dwarf, together normally 10.247 mag (V), prototype of the T CrB stars (see "[[Suggested Stellar Transients\|Transients]]"). Occasionally, the system permits nova eruptions (surface eruptions on the white dwarf), which flare it up to mag 3 or 2. Although its usual brightness is below the detection limit of the human eye, the star is included in the Yale Bright Star Catalog because of its peak magnitude.		The name "Blaze Star" as a nickname for the eruptive variable T CrB ([https://simbad.cds.unistra.fr/simbad/sim-basic?Ident=T+CrB&submit=SIMBAD+search Simbad], [https://vsx.aavso.org/index.php?view=detail.top&oid=10602 VSX]) has been used since the 19th century. The symbiotic system in [[Corona Borealis]] consists of a red giant and a white dwarf, together normally 10.247 mag (V), prototype of the T CrB stars (see "[[Suggested Stellar Transients\|Transients]]"). Occasionally, the system permits nova eruptions (surface eruptions on the white dwarf), which flare it up to mag 3 or 2. Although its usual brightness is below the detection limit of the human eye, the star is included in the Yale Bright Star Catalog because of its peak magnitude.

	==Concordance, Etymology, History==		==Concordance, Etymology, History==
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	=== Specifically on T CrB ===		=== Specifically on T CrB ===
	[[File:TCrB aavsoLCG2 2024.jpg\|thumb\|A light curve of T CrB based on the data archive of the [https://www.aavso.org/LCGv2/ AAVSO] (2024).]]		[[File:TCrB aavsoLCG2 2024.jpg\|thumb\|A light curve of T CrB based on the data archive of the [https://www.aavso.org/LCGv2/ AAVSO] (2024).]]
	In 2024/ 2025, ~~the~~ press ~~campaigns~~ claimed that the star will erupt soon because the last eruption of T CrB was about 80 years ago, i.e., in 1946. If we think carefully about how many survey programs and systematic sky monitoring observation programs there were at the end of World War II, we can't think of many. At that time, there were no satellite telescopes, and the culture of observational astronomy consisted mainly of individual stargazers who, while observing their favourite objects, might have found an erupting star “by chance.”		In 2024/2025, press reports claimed that the star will erupt soon because the last eruption of T CrB was about 80 years ago, i.e., in 1946. If we think carefully about how many survey programs and systematic sky monitoring observation programs there were at the end of World War II, we can't think of many. At that time, there were no satellite telescopes, and the culture of observational astronomy consisted mainly of individual stargazers who, while observing their favourite objects, might have found an erupting star “by chance.”

	It was no different ''before'' World War II. So how do we know the recurrence period? It is clearly visible that there is a huge data gap between 1870 and 1930.		It was no different ''before'' World War II. So how do we know the recurrence period? It is clearly visible that there is a huge data gap between 1870 and 1930.


	==Mythology==		==Mythology==
	no mythology		no mythology
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	== Reference ==		== Reference ==
	* [[References\|References (general)]]		* [[References\|References (general)]]
	* Ian Ridpath's website ([http://ianridpath.com/startales Star Tales] )		* Ian Ridpath's website ([http://www.ianridpath.com/startales/coronaborealis.html#blaze Star Tales, Corona Borealis] )

	[[Category:IAU-Star Name‏‎]]		[[Category:IAU-Star Name‏‎]]

IanRidpath: Copyedit

2026-02-18T08:41:20Z

Copyedit

Sushoff at 20:17, 31 January 2026

2026-01-31T20:17:04Z

← Older revision		Revision as of 20:17, 31 January 2026
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	The observers agree that in this region of the sky near the galactic pole, where there are few bright stars, it “disturbed”/ “distorted” the shape of the constellation (as they say). The nova was therefore definitely conspicuous and could be identified as a star of magnitude 9.5 in the Bonn survey. This made it clear that this “new star” was an eruption of a known one.		The observers agree that in this region of the sky near the galactic pole, where there are few bright stars, it “disturbed”/ “distorted” the shape of the constellation (as they say). The nova was therefore definitely conspicuous and could be identified as a star of magnitude 9.5 in the Bonn survey. This made it clear that this “new star” was an eruption of a known one.
			[[File:Proctor1872 StarDepths blazeStar.png\|thumb\|"Blaze Star" in Proctor's note on "star depths" in 1872.]]
	Back then—in 1866—people didn't even know how stars work or where the sun gets its energy from, let alone how stars evolve or why some of them change brightness. They saw it, recorded their observations—and didn't (yet) understand it.		Back then—in 1866—people didn't even know how stars work or where the sun gets its energy from, let alone how stars evolve or why some of them change brightness. They saw it, recorded their observations—and didn't (yet) understand it.

Sushoff at 20:14, 31 January 2026

2026-01-31T20:14:20Z

← Older revision		Revision as of 20:14, 31 January 2026
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	=== Occurance of the Name ===		=== Occurance of the Name ===
	WGSN found that the first recorded use of the name Blaze Star for T CrB was in a lecture by the British spectroscopist William Allen Miller at a meeting of the British Association in 1869, and published in the ''English Mechanic''. The name was popularized by R. A. Proctor (1872) and later his daughter Mary Proctor (1897).		The nickname has been around since the late 19th century, and it propagated in astronomy literature significantly since then. WGSN found that the first recorded use of the name Blaze Star for T CrB was in a lecture by the British spectroscopist William Allen Miller at a meeting of the British Association in 1869, and published in the ''English Mechanic''. The name was popularized by R. A. Proctor (1872, see [https://books.google.de/books?id=bLJXAAAAYAAJ&pg=PA378&dq=Coronae+%22Blaze+star%22&hl=en&newbks=1&newbks_redir=0&sa=X&redir_esc=y#v=onepage&q=Coronae%20%22Blaze%20star%22&f=true GoogleBooks])<ref>Proctor, Richard A. (1872). The star depths. The Mechanics' Magazine, 96, 378-379.</ref> and later his daughter Mary Proctor (1897, see [https://articles.adsabs.harvard.edu/pdf/1897PA......5...97P on adsabs], p.104).
			[[File:Blaze Star ProctorMary.png\|thumb\|Screenshot from [https://articles.adsabs.harvard.edu/pdf/1897PA......5...97P Mary Proctor's paper] (CC BY Ian Ridpath).]]
			Note that the [https://ui.adsabs.harvard.edu/search/fq=%7B!type%3Daqp%20v%3D%24fq_database%7D&fq_database=(database%3Aastronomy%20OR%20database%3Aphysics)&p_=0&q=%22Blaze%20Star%22&sort=date%20asc%2C%20bibcode%20asc earliest paper] [https://ui.adsabs.harvard.edu/search/fq=%7B!type%3Daqp%20v%3D%24fq_database%7D&fq_database=(database%3Aastronomy%20OR%20database%3Aphysics)&p_=0&q=%22Blaze%20Star%22&sort=date%20asc%2C%20bibcode%20asc in the 1880s] that speaks of a "Blazing Star" deals with zeta Cassiopeiae (1886). Sara Schechner in the 1990s (e.g. [https://ui.adsabs.harvard.edu/#abs/1990taa..conf....9S/abstract Schechner 1990]) still uses the term in a general sense and not as a proper name.
			[[File:BlazeStar Capture.jpg\|center\|thumb\|800x800px]]
			However, thename "Blaze Star" for the specific object in Corona Borealis is first found in the note in the [https://books.google.com/books?id=xj48AQAAMAAJ&pg=PA515 English Mechanic and Mirror Science in September 1869], displayed above.

	=== Expections for next eruption ===		=== Expections for next eruption ===
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	=== Physics of Recurrent Novae ===		=== Physics of Recurrent Novae ===
			<div style="float:right; margin:0 0 1em 1em;">
			<youtube align=right>https://youtu.be/DB6IMc_g1QU</youtube>
			</div>
	A nova eruption is a surface eruption on a star in a cataclysmic binary star system. These are star systems in which the two stars orbit each other so closely that matter flows from the primary star (donor) to the companion star. The donor can be a red giant star, but it can also be a yellow main sequence star or even a white dwarf. In most cases, the receiving and occasionally erupting “star” is a white dwarf, i.e., the remnant of a sun-like star (i.e., no longer a star itself because it no longer gains energy through nuclear fusion in its interior).		A nova eruption is a surface eruption on a star in a cataclysmic binary star system. These are star systems in which the two stars orbit each other so closely that matter flows from the primary star (donor) to the companion star. The donor can be a red giant star, but it can also be a yellow main sequence star or even a white dwarf. In most cases, the receiving and occasionally erupting “star” is a white dwarf, i.e., the remnant of a sun-like star (i.e., no longer a star itself because it no longer gains energy through nuclear fusion in its interior).

Sushoff at 19:41, 31 January 2026

2026-01-31T19:41:31Z

← Older revision		Revision as of 19:41, 31 January 2026
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	==Concordance, Etymology, History==		==Concordance, Etymology, History==
	On May 12, 1866, at least three observers were the first to observe a star at this location in the sky ([https://iopscience.iop.org/article/10.1086/125797/pdf PDF]).
			=== Discovery ===
			On May 12, 1866, at least three observers were the first to observe a star at this location in the sky ([https://iopscience.iop.org/article/10.1086/125797/pdf Petit 1946, PDF]).

	# The director of the Athens Observatory, Mr. Schmidt, saw the star with a magnitude of 5 during a sky survey between 8:30 p.m. and 9:45 p.m. (local time).		# The director of the Athens Observatory, Mr. Schmidt, saw the star with a magnitude of 5 during a sky survey between 8:30 p.m. and 9:45 p.m. (local time).
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	'''Note:''' We have no less than two data points (nova light curves) from the star whose eruption we are now expecting. One of these dates back to before the invention of electrical photometry (Potsdam, 1913), i.e., it is based solely on the estimates of experienced observers: a well-functioning method, but not using the same measurement method we use today. Contrary to everything taught in basic physics courses (or any laboratory course), we have no choice but to compare measurements that school physics teaches us are not comparable (common practice in astronomy).		'''Note:''' We have no less than two data points (nova light curves) from the star whose eruption we are now expecting. One of these dates back to before the invention of electrical photometry (Potsdam, 1913), i.e., it is based solely on the estimates of experienced observers: a well-functioning method, but not using the same measurement method we use today. Contrary to everything taught in basic physics courses (or any laboratory course), we have no choice but to compare measurements that school physics teaches us are not comparable (common practice in astronomy).

			=== Occurance of the Name ===
			WGSN found that the first recorded use of the name Blaze Star for T CrB was in a lecture by the British spectroscopist William Allen Miller at a meeting of the British Association in 1869, and published in the ''English Mechanic''. The name was popularized by R. A. Proctor (1872) and later his daughter Mary Proctor (1897).

	=== Expections for next eruption ===		=== Expections for next eruption ===

Sushoff at 15:57, 20 January 2026

2026-01-20T15:57:33Z

← Older revision		Revision as of 15:57, 20 January 2026
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			Authors: {{PAGEAUTHORS}}
			----
	[[File:EnglishMechanicAndMirrorOfScience1869 content hi.jpg\|thumb\|screenshot of a page in the English Mechanic and Mirror Science, Sept 1869 - Here, the name "Blaze Star, 1866" is chosen as a headline]]		[[File:EnglishMechanicAndMirrorOfScience1869 content hi.jpg\|thumb\|screenshot of a page in the English Mechanic and Mirror Science, Sept 1869 - Here, the name "Blaze Star, 1866" is chosen as a headline]]
	[[File:TCrB bsc1990-768x485.jpg\|thumb\|The variable star T CrB is included in the Yale Bright Star Catalog (HR 5859), here depicted in a star chart in Hoffmann (2017).]]		[[File:TCrB bsc1990-768x485.jpg\|thumb\|The variable star T CrB is included in the Yale Bright Star Catalog (HR 5859), here depicted in a star chart in Hoffmann (2017).]]

Sushoff: /* IAU Working Group on Star Names */

2025-10-01T10:21:30Z

IAU Working Group on Star Names

← Older revision		Revision as of 10:21, 1 October 2025
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	==IAU Working Group on Star Names==		==IAU Working Group on Star Names==
	The name was discussed by the IAU WGSN in ~~2025~~ due to the ongoing media hype on its due eruption. ~~No decision yet~~. <gallery>		The name was discussed by the IAU WGSN in 2024 due to the ongoing media hype on its due eruption. It was adopted in September 2025. <gallery>
	File:Blaze Star profileCard SadeghFaghanpour-IAU-WGSN.jpg\|Blaze Star, profile card, (CC BY Sadegh Faganpour for WGSN 2025).		File:Blaze Star profileCard SadeghFaghanpour-IAU-WGSN.jpg\|Blaze Star, profile card, (CC BY Sadegh Faganpour for WGSN 2025).
	File:Blaze Star stickfigure SadeghFaghanpour-IAU-WGSN.jpg\|Blaze Star, stick figure, (CC BY Sadegh Faganpour for WGSN 2025).		File:Blaze Star stickfigure SadeghFaghanpour-IAU-WGSN.jpg\|Blaze Star, stick figure, (CC BY Sadegh Faganpour for WGSN 2025).

Sushoff at 17:23, 30 September 2025

2025-09-30T17:23:32Z

← Older revision		Revision as of 17:23, 30 September 2025
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	[[File:EnglishMechanicAndMirrorOfScience1869 content hi.jpg\|thumb\|screenshot of a page in the English Mechanic and Mirror Science, Sept 1869 - Here, the name "Blaze Star, 1866" is chosen as a headline]]		[[File:EnglishMechanicAndMirrorOfScience1869 content hi.jpg\|thumb\|screenshot of a page in the English Mechanic and Mirror Science, Sept 1869 - Here, the name "Blaze Star, 1866" is chosen as a headline]]
	[[File:TCrB bsc1990-768x485.jpg\|thumb\|The variable star T CrB is included in the Yale Bright Star Catalog (HR 5859), here depicted in a star chart in Hoffmann (2017).]]		[[File:TCrB bsc1990-768x485.jpg\|thumb\|The variable star T CrB is included in the Yale Bright Star Catalog (HR 5859), here depicted in a star chart in Hoffmann (2017).]]
	The name "Blaze Star" as a nickname for T CrB ([https://simbad.cds.unistra.fr/simbad/sim-basic?Ident=T+CrB&submit=SIMBAD+search Simbad], [https://vsx.aavso.org/index.php?view=detail.top&oid=10602 VSX]) in eruption; it is being used since the 19th century. The symbiotic system consists of a red giant and a white dwarf, together normally 10.247 mag bright (V). Occasionally, the system permits nova eruptions (surface eruptions on the white dwarf) which flare it up to mag 3 or 2. Although its usual brightness is below the detection limit of the human eye, the star is included in the Yale Bright Star Catalog (because of its peak magnitude).		The name "Blaze Star" as a nickname for T CrB ([https://simbad.cds.unistra.fr/simbad/sim-basic?Ident=T+CrB&submit=SIMBAD+search Simbad], [https://vsx.aavso.org/index.php?view=detail.top&oid=10602 VSX]) in eruption; it is being used since the 19th century. The symbiotic system in [[Corona Borealis]] consists of a red giant and a white dwarf, together normally 10.247 mag bright (V), prototype of the T CrB-stars (see "[[Suggested Stellar Transients\|Transients]]"). Occasionally, the system permits nova eruptions (surface eruptions on the white dwarf), which flare it up to mag 3 or 2. Although its usual brightness is below the detection limit of the human eye, the star is included in the Yale Bright Star Catalog (because of its peak magnitude).

	==Concordance, Etymology, History==		==Concordance, Etymology, History==
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	=== Expections for next eruption ===		=== Expections for next eruption ===
	Three of the other T CrB-class star systems erupt somewhat more frequently: every 20 to 30 years, so that what the press tells us about the impending eruption may not be entirely reliable. We suspect that during the outburst, the star will have approximately the brightness (3 to 2 mag) of the North Star or the main star of a constellation (alf CrB, Alphecca), because this was the case in both documented observations. Many (50%) recurrent novae always erupt with the same brightness – but the peak brightness can also vary (the other 50%). Therefore, it cannot be completely ruled out that the star T CrB will not be quite as bright as last time (e.g., only 4 mag or even only 6 mag) or that it will be even brighter (up to Arcturus brightness) during its upcoming outburst: We will only know for sure when we see it.		Three of the other T CrB-class star systems erupt somewhat more frequently: every 20 to 30 years, so that what the press tells us about the impending eruption may not be entirely reliable. We suspect that during the outburst, the star will have approximately the brightness (3 to 2 mag) of the North Star or the main star of a constellation (alf CrB, [[Alphecca]]), because this was the case in both documented observations. Many (50%) recurrent novae always erupt with the same brightness – but the peak brightness can also vary (the other 50%). Therefore, it cannot be completely ruled out that the star T CrB will not be quite as bright as last time (e.g., only 4 mag or even only 6 mag) or that it will be even brighter (up to Arcturus brightness) during its upcoming outburst: We will only know for sure when we see it.

	=== Physics of Recurrent Novae ===		=== Physics of Recurrent Novae ===

Sushoff at 16:57, 30 September 2025

2025-09-30T16:57:04Z

← Older revision		Revision as of 16:57, 30 September 2025
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	[[Category:IAU-Star Name‏‎]]		[[Category:IAU-Star Name‏‎]]
	[[Category:Star Name‏‎]]		[[Category:Star Name‏‎]]
			[[Category:Transient]]
	[[Category:Modern]]		[[Category:Modern]]
	[[Category:CrB]]		[[Category:CrB]]

← Older revision		Revision as of 08:41, 18 February 2026
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	[[File:EnglishMechanicAndMirrorOfScience1869 content hi.jpg\|thumb\|screenshot of a page in the English Mechanic and Mirror Science, Sept 1869 - Here, the name "Blaze Star, 1866" is chosen as a headline]]		[[File:EnglishMechanicAndMirrorOfScience1869 content hi.jpg\|thumb\|screenshot of a page in the English Mechanic and Mirror Science, Sept 1869 - Here, the name "Blaze Star, 1866" is chosen as a headline]]
	[[File:TCrB bsc1990-768x485.jpg\|thumb\|The variable star T CrB is included in the Yale Bright Star Catalog (HR 5859), here depicted in a star chart in Hoffmann (2017).]]		[[File:TCrB bsc1990-768x485.jpg\|thumb\|The variable star T CrB is included in the Yale Bright Star Catalog (HR 5859), here depicted in a star chart in Hoffmann (2017).]]
	The name "Blaze Star" as a nickname for T CrB ([https://simbad.cds.unistra.fr/simbad/sim-basic?Ident=T+CrB&submit=SIMBAD+search Simbad], [https://vsx.aavso.org/index.php?view=detail.top&oid=10602 VSX]) ~~in eruption; it is being~~ used since the 19th century. The symbiotic system in [[Corona Borealis]] consists of a red giant and a white dwarf, together normally 10.247 mag ~~bright~~ (V), prototype of the T CrB-stars (see "[[Suggested Stellar Transients\|Transients]]"). Occasionally, the system permits nova eruptions (surface eruptions on the white dwarf), which flare it up to mag 3 or 2. Although its usual brightness is below the detection limit of the human eye, the star is included in the Yale Bright Star Catalog (because of its peak magnitude).		The name "Blaze Star" as a nickname for the eruptive variable T CrB ([https://simbad.cds.unistra.fr/simbad/sim-basic?Ident=T+CrB&submit=SIMBAD+search Simbad], [https://vsx.aavso.org/index.php?view=detail.top&oid=10602 VSX]) ha sbeen used since the 19th century. The symbiotic system in [[Corona Borealis]] consists of a red giant and a white dwarf, together normally 10.247 mag (V), prototype of the T CrB stars (see "[[Suggested Stellar Transients\|Transients]]"). Occasionally, the system permits nova eruptions (surface eruptions on the white dwarf), which flare it up to mag 3 or 2. Although its usual brightness is below the detection limit of the human eye, the star is included in the Yale Bright Star Catalog because of its peak magnitude.

	==Concordance, Etymology, History==		==Concordance, Etymology, History==
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	# and W. J. Lynn from the Greenwich Observatory in London saw the object a little later (between 11:30 p.m. and 11:45 p.m.) on his way (not from an observatory) even with the naked eye, because it was already as bright as the main star of the constellation (magnitude 2.2).		# and W. J. Lynn from the Greenwich Observatory in London saw the object a little later (between 11:30 p.m. and 11:45 p.m.) on his way (not from an observatory) even with the naked eye, because it was already as bright as the main star of the constellation (magnitude 2.2).

	In some sources, Birmingham is given as the first but as Ireland is further west and north than Athens, he must have seen the nova later. Civil twilight ends only at roughly 22:10 on Tuam ~~island~~ on the 12th of May, so he could have seen the nova only some hours after any observer in Athens (due to timezone difference and much later end of twilight).		In some sources, Birmingham is given as the first but as Ireland is further west and north than Athens he must have seen the nova later. Civil twilight ends only at roughly 22:10 on Tuam in western Ireland on the 12th of May, so he could have seen the nova only some hours after any observer in Athens (due to timezone difference and much later end of twilight).

	The observers agree that in this region of the sky near the galactic pole, where there are few bright stars, it “disturbed”/ “distorted” the shape of the constellation ~~(as they say)~~. The nova was therefore definitely conspicuous and could be identified as a star of magnitude 9.5 in the Bonn survey. This made it clear that this “new star” was an eruption of a known one.		The observers agree that in this region of the sky near the galactic pole, where there are few bright stars, it “disturbed”/ “distorted” the shape of the constellation. The nova was therefore definitely conspicuous and could be identified as a star of magnitude 9.5 in the Bonn survey. This made it clear that this “new star” was an eruption of a known one.
	[[File:Proctor1872 StarDepths blazeStar.png\|thumb\|"Blaze Star" in Proctor's note on "star depths" in 1872.]]		[[File:Proctor1872 StarDepths blazeStar.png\|thumb\|"Blaze Star" in Proctor's note on "star depths" in 1872.]]
	Back then—in 1866—people didn't even know how stars work or where the ~~sun~~ gets its energy from, let alone how stars evolve or why some of them change brightness. They saw it, recorded their observations—and didn't (yet) understand it.		Back then—in 1866—people didn't even know how stars work or where the Sun gets its energy from, let alone how stars evolve or why some of them change brightness. They saw it, recorded their observations—and didn't (yet) understand it.

	It was not until 1946 that the next bright flare was seen, and in the intervening period, apparently (almost) no one looked at this star – at least, there are no observation data in the data archive (but the light curve also begins in 1866 only after the flare has subsided (at 7 mag).		It was not until 1946 that the next bright flare was seen, and in the intervening period, apparently (almost) no one looked at this star – at least, there are no observation data in the data archive (but the light curve also begins in 1866 only after the flare has subsided (at 7 mag).
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	=== Occurance of the Name ===		=== Occurance of the Name ===
	The nickname has been around since the late 19th century, and it propagated in astronomy literature significantly since then. WGSN found that the first recorded use of the name Blaze Star for T CrB was in a lecture by the British spectroscopist William Allen Miller at a meeting of the British Association in 1869, and published in the ''English Mechanic''. The name was popularized by R. A. Proctor (1872, see [https://books.google.de/books?id=bLJXAAAAYAAJ&pg=PA378&dq=Coronae+%22Blaze+star%22&hl=en&newbks=1&newbks_redir=0&sa=X&redir_esc=y#v=onepage&q=Coronae%20%22Blaze%20star%22&f=true GoogleBooks])<ref>Proctor, Richard A. (1872). The star depths. The Mechanics' Magazine, 96, 378-379.</ref> and later his daughter Mary Proctor (1897, see [https://articles.adsabs.harvard.edu/pdf/1897PA......5...97P on adsabs], p.104).		The nickname has been around since the late 19th century, and it has propagated in astronomy literature significantly since then. WGSN found that the first recorded use of the name Blaze Star for T CrB was in a lecture by the British spectroscopist William Allen Miller at a meeting of the British Association in 1869, and published in the ''English Mechanic''. The name was popularized by R. A. Proctor (1872, see [https://books.google.de/books?id=bLJXAAAAYAAJ&pg=PA378&dq=Coronae+%22Blaze+star%22&hl=en&newbks=1&newbks_redir=0&sa=X&redir_esc=y#v=onepage&q=Coronae%20%22Blaze%20star%22&f=true GoogleBooks])<ref>Proctor, Richard A. (1872). The star depths. The Mechanics' Magazine, 96, 378-379.</ref> and later his daughter Mary Proctor (1897, see [https://articles.adsabs.harvard.edu/pdf/1897PA......5...97P on adsabs], p.104).
	[[File:Blaze Star ProctorMary.png\|thumb\|Screenshot from [https://articles.adsabs.harvard.edu/pdf/1897PA......5...97P Mary Proctor's paper] (CC BY Ian Ridpath).]]		[[File:Blaze Star ProctorMary.png\|thumb\|Screenshot from [https://articles.adsabs.harvard.edu/pdf/1897PA......5...97P Mary Proctor's paper] (CC BY Ian Ridpath).]]
	Note that the [https://ui.adsabs.harvard.edu/search/fq=%7B!type%3Daqp%20v%3D%24fq_database%7D&fq_database=(database%3Aastronomy%20OR%20database%3Aphysics)&p_=0&q=%22Blaze%20Star%22&sort=date%20asc%2C%20bibcode%20asc earliest paper] [https://ui.adsabs.harvard.edu/search/fq=%7B!type%3Daqp%20v%3D%24fq_database%7D&fq_database=(database%3Aastronomy%20OR%20database%3Aphysics)&p_=0&q=%22Blaze%20Star%22&sort=date%20asc%2C%20bibcode%20asc in the 1880s] that speaks of a "Blazing Star" deals with ~~zeta~~ Cassiopeiae (1886). Sara Schechner in the 1990s (e.g. [https://ui.adsabs.harvard.edu/#abs/1990taa..conf....9S/abstract Schechner 1990]) still uses the term in a general sense and not as a proper name.		Note that the [https://ui.adsabs.harvard.edu/search/fq=%7B!type%3Daqp%20v%3D%24fq_database%7D&fq_database=(database%3Aastronomy%20OR%20database%3Aphysics)&p_=0&q=%22Blaze%20Star%22&sort=date%20asc%2C%20bibcode%20asc earliest paper] [https://ui.adsabs.harvard.edu/search/fq=%7B!type%3Daqp%20v%3D%24fq_database%7D&fq_database=(database%3Aastronomy%20OR%20database%3Aphysics)&p_=0&q=%22Blaze%20Star%22&sort=date%20asc%2C%20bibcode%20asc in the 1880s] that speaks of a "Blazing Star" deals with Zeta Cassiopeiae (1886). Sara Schechner in the 1990s (e.g. [https://ui.adsabs.harvard.edu/#abs/1990taa..conf....9S/abstract Schechner 1990]) still uses the term in a general sense and not as a proper name.
	[[File:BlazeStar Capture.jpg\|center\|thumb\|800x800px]]		[[File:BlazeStar Capture.jpg\|center\|thumb\|800x800px]]
	However, thename "Blaze Star" for the specific object in Corona Borealis is first found in the note in the [https://books.google.com/books?id=xj48AQAAMAAJ&pg=PA515 English Mechanic and Mirror Science in September 1869], displayed above.		However, thename "Blaze Star" for the specific object in Corona Borealis is first found in the note in the [https://books.google.com/books?id=xj48AQAAMAAJ&pg=PA515 English Mechanic and Mirror Science in September 1869], displayed above.