Blaze Star: Difference between revisions
(Created page with "The name "Blaze Star" as a nickname for T CrB in eruption is being used since the 19th century. ==Concordance, Etymology, History== ==Mythology== no mythology ==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. == Weblinks == * == Reference == * References (general) * Ian Ridpath's website ([http://ianridpath.com/startales Star Tales] ) Catego...") Tag: Disambiguation links |
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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]] |
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The name "Blaze Star" as a nickname for T CrB in eruption is being used since the 19th century. |
The name "Blaze Star" as a nickname for T CrB in eruption is being used since the 19th century. |
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==Concordance, Etymology, History== |
==Concordance, Etymology, History== |
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=== Physics === |
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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). |
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In most cases, we know of at most one eruption as a classic nova from these cataclysmic (or symbiotic) systems. However, there are 30 stars (as of May 5, 2024) that are known or suspected to be “recurrent” novae; twelve of them are outside the Milky Way (galaxy), eight are uncertain. |
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So we only have ten objects of this type that we can study in more detail in order to make further statistical statements about their behavior – and predictions! |
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In astronomy, the obvious characteristics of a system are used for classification. In the case of our recurrent novae, these would be the orbital period (period duration) Porb, the amplitude A during eruption, the repetition time τ<sub>r</sub>, and the decay time t<sub>3</sub> from the maximum of 3 mag. The period depends on the size of the main star (donor): with a small donor, the orbiting dwarf star must be closer so that matter can flow over, and therefore it has a shorter period due to Kepler's laws. |
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Characterization of the ten known recurrent novae: In T Pyx stars, the erupting star orbits a dwarf star (blue), in U Sco types it orbits a main sequence star (yellow), and in T CrB types it orbits a red giant. |
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==Mythology== |
==Mythology== |
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Revision as of 11:16, 17 September 2025
The name "Blaze Star" as a nickname for T CrB in eruption is being used since the 19th century.
Concordance, Etymology, History
Physics
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).
In most cases, we know of at most one eruption as a classic nova from these cataclysmic (or symbiotic) systems. However, there are 30 stars (as of May 5, 2024) that are known or suspected to be “recurrent” novae; twelve of them are outside the Milky Way (galaxy), eight are uncertain.
So we only have ten objects of this type that we can study in more detail in order to make further statistical statements about their behavior – and predictions!
In astronomy, the obvious characteristics of a system are used for classification. In the case of our recurrent novae, these would be the orbital period (period duration) Porb, the amplitude A during eruption, the repetition time τr, and the decay time t3 from the maximum of 3 mag. The period depends on the size of the main star (donor): with a small donor, the orbiting dwarf star must be closer so that matter can flow over, and therefore it has a shorter period due to Kepler's laws.
Characterization of the ten known recurrent novae: In T Pyx stars, the erupting star orbits a dwarf star (blue), in U Sco types it orbits a main sequence star (yellow), and in T CrB types it orbits a red giant.
Mythology
no mythology
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.
Weblinks
Reference
- References (general)
- Ian Ridpath's website (Star Tales )
