Irregular variable: Difference between revisions

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{{Short description|Type of variable star}}

An '''irregular variable''' is a type of [[variable star]] in which variations in brightness show no regular [[periodicity]]. There are two main sub-types of irregular variable: eruptive and pulsating.

{{Refimprove|date=December 2009}}

An '''irregular variable''' is a type of [[variable star]] in which variations in brightness show no regular [[Frequency|periodicity]]. There are two main sub-types of irregular variable: eruptive and pulsating.

'''Eruptive''' irregular variables are divided into three categories:

* Group I variables are split into subgroups IA (spectral types O to A) and IB (spectral types F through M).

* [[Orion variables]], GCVS type IN (irregular and nebulous), indigenous to star-forming regions, may vary by several magnitudes with rapid changes of up to 1 magnitude in 1 to 10 days, are similarly divided by spectral type into subgroups INA and INB, but with the addition of another subgroup, INT, for [[T Tauri starsstar]]s, or INT(YY) for YY Orionis stars.

* The third category of eruptive irregulars are the IS stars, which show rapid variations of 0.5 to 1 magnitude in a few hours or days; again, these come in subgroups ISA and ISB.

'''Pulsating''' irregular giants or supergiants, called [[slow irregular variable]]s, are all of late spectral types (K, M, C, or S), and classed as type L-LB for giants and LC for supergiants. How many of these are actually semi-regular variables that simply need more study, remains unclear.<ref>{{citation|title=Observing Variable Stars |author=Gerry Arlen Good|year= 2003|publisher=Springer Science|url= httphttps://books.google.com/books?vid=ISBN1852334983&id=k9ViYKvKRz0C&pg=PA8&lpg=PA8&ots=AojoVu3Lpn&dqq=%22Irregular+variable%22&iepg=ISO-8859PA8|isbn=978-1&output=html&sig=hIF3ZDs-Rh3XGKVECqONh7aKAYM|id=ISBN 185233498385233-498-7}}</ref>

* [[Orion variables]], GCVS type IN (irregular and nebulous), indigenous to star-forming regions, may vary by several magnitudes with rapid changes of up to 1 magnitude in 1 to 10 days, are similarly divided by spectral type into subgroups INA and INB, but with the addition of another subgroup, INT, for T Tauri stars, or INT(YY) for YY Orionis stars.

== References ==

* The third category of eruptive irregulars are the IS stars, which show rapid variations of 0.5 to 1 magnitude in a few hours or days; again, these come in subgroups ISA and ISB.

{{Reflist}}

[[Category:Irregular variables| ]]

'''Pulsating''' irregular giants or supergiants, called [[slow irregular variable]]s, are all of late spectral types (K, M, C, or S), and classed as type L-LB for giants and LC for supergiants. How many of these are actually semi-regular variables that simply need more study, remains unclear.<ref>{{citation|title=Observing Variable Stars |author=Gerry Arlen Good|year= 2003|publisher=Springer Science|url= http://books.google.com/books?vid=ISBN1852334983&id=k9ViYKvKRz0C&pg=PA8&lpg=PA8&ots=AojoVu3Lpn&dq=%22Irregular+variable%22&ie=ISO-8859-1&output=html&sig=hIF3ZDs-Rh3XGKVECqONh7aKAYM|id=ISBN 1852334983}}</ref>

==References==

<references />

[[Category:Irregular variables]]

{{var-star-stub}}

[[ca:Estrella variable irregular]]

[[es:Estrella variable irregular]]

[[fr:Variable irrégulière]]

[[it:Variabile irregolare]]

[[pl:Gwiazda zmienna nieregularna]]

[[sk:Nepravidelná premenná hviezda]]

[[zh:不規則變星]]