Be X-ray Binaries - Revision history

Zainab at 11:16, 16 November 2023

2023-11-16T11:16:41Z

Zainab at 10:54, 16 November 2023

2023-11-16T10:54:28Z

Stierhof at 14:50, 4 July 2022

2022-07-04T14:50:40Z

Stierhof at 14:50, 4 July 2022

2022-07-04T14:50:25Z

Kuehnel at 13:12, 13 April 2018

2018-04-13T13:12:02Z

Kuehnel at 15:43, 12 April 2018

2018-04-12T15:43:58Z

Kuehnel at 09:30, 12 April 2018

2018-04-12T09:30:11Z

Kuehnel: Created page with " Category:Accreting X-ray Pulsars Be/X-ray binary systems form the majority of accreting X-ray pulsars. In these systems the optical companion is a giant star which besi..."

2018-04-12T08:19:42Z

Created page with " Category:Accreting X-ray Pulsars Be/X-ray binary systems form the majority of accreting X-ray pulsars. In these systems the optical companion is a giant star which besi..."

New page

[[Category:Accreting X-ray Pulsars]]

Be/X-ray binary systems form the majority of accreting X-ray pulsars. In these systems the optical companion is a giant star which besides a fast low-density wind also show an equatorial disk or flattened envelope in fast rotation. This disk shows up through [http://en.wikipedia.org/wiki/Balmer_lines Balmer emission lines] (see, e.g., [http://www.astrosurf.com/~buil/us/bestar.htm The spectroscopic Be stars Atlas]. The X-ray emitting object is usually a neutron star on an eccentric orbit (e=0.1-0.9). For a recent review of Be/X-ray binaries see Reig et al. (2011)<ref name = "Reig2011a" />.

Most Be/X-ray binaries show transient activity and only very weak emission outside outbursts. Stella et al. (1986)<ref name = "Stella1986" /> have classified the different outbursts in two types: Type I are periodical outbursts linked to the periastron passage of the neutron star and relatively short; Type II are larger outbursts with no clear link to the orbital phase.

Historically, type I outbursts have been explained by a simple picture of the passage of the neutron star through the equatorial disk of the Be star every orbit. But this picture fails to explain the large variety of outbursts seen in many systems with periods of regular outbursts, occasional giant outbursts, but also extended periods of quiescence. A possible explanation was given by the [http://harmas.arc.hokkai-s-u.ac.jp/~okazaki/BeX/index.html model developed by Atsuo Okazaki] in which the disk around the Be star will often be truncated due to tidal interactions and outbursts are triggered by changes in the disk. This model has been published in Negueruela & Okazaki 2001<ref name = "Negueruela2001a" />, Negueruela (2001)<ref name = "Negueruela2001a" />, and Okazaki & Negueruela (2001)<ref name = "Okazaki2001a" />.

[http://integral.esac.esa.int/bexrbmonitor/webpage_oneplot.php The BeXRB Monitor] page collects data from different monitoring missions and shows current activity for a variety of sources.

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 Historically, type I outbursts have been explained by a simple picture of the passage of the neutron star through the equatorial disk of the Be star every orbit. But this picture fails to explain the large variety of outbursts seen in many systems with periods of regular outbursts, occasional giant outbursts, but also extended periods of quiescence. A possible explanation was given by the [http://harmas.arc.hokkai-s-u.ac.jp/~okazaki/BeX/index.html model developed by Atsuo Okazaki] in which the disk around the Be star will often be truncated due to tidal interactions and outbursts are triggered by changes in the disk. This model has been published in Negueruela & Okazaki 2001<ref name = "Negueruela2001a" />, Negueruela et al. (2001)<ref name = "Negueruela2001b" />, and Okazaki & Negueruela (2001)<ref name = "Okazaki2001a" />.
-Sometimes, optical information can prove quite useful while studying BeXRBs. Check [[Be stars in Gaia]] for a few simple checks.
+Sometimes, optical information can prove quite useful while studying BeXRBs. See [[Be stars in Gaia]] for a few simple checks.
 [http://integral.esac.esa.int/bexrbmonitor/webpage_oneplot.php The BeXRB Monitor] page collects data from different monitoring missions and shows current activity for a variety of sources.
 See [[List of Be X-ray Binaries]] for details about individual sources.

@@ Line 8: / Line 8: @@
 Historically, type I outbursts have been explained by a simple picture of the passage of the neutron star through the equatorial disk of the Be star every orbit. But this picture fails to explain the large variety of outbursts seen in many systems with periods of regular outbursts, occasional giant outbursts, but also extended periods of quiescence. A possible explanation was given by the [http://harmas.arc.hokkai-s-u.ac.jp/~okazaki/BeX/index.html model developed by Atsuo Okazaki] in which the disk around the Be star will often be truncated due to tidal interactions and outbursts are triggered by changes in the disk. This model has been published in Negueruela & Okazaki 2001<ref name = "Negueruela2001a" />, Negueruela et al. (2001)<ref name = "Negueruela2001b" />, and Okazaki & Negueruela (2001)<ref name = "Okazaki2001a" />.
 [http://integral.esac.esa.int/bexrbmonitor/webpage_oneplot.php The BeXRB Monitor] page collects data from different monitoring missions and shows current activity for a variety of sources.
 See [[List of Be X-ray Binaries]] for details about individual sources.

← Older revision		Revision as of 14:50, 4 July 2022
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	See [[List of Be X-ray Binaries]] for details about individual sources.		See [[List of Be X-ray Binaries]] for details about individual sources.
−
−	~~{{List of References}}~~

← Older revision		Revision as of 14:50, 4 July 2022
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	See [[List of Be X-ray Binaries]] for details about individual sources.		See [[List of Be X-ray Binaries]] for details about individual sources.
		+
		+	{{List of References}}

← Older revision		Revision as of 13:12, 13 April 2018
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	[http://integral.esac.esa.int/bexrbmonitor/webpage_oneplot.php The BeXRB Monitor] page collects data from different monitoring missions and shows current activity for a variety of sources.		[http://integral.esac.esa.int/bexrbmonitor/webpage_oneplot.php The BeXRB Monitor] page collects data from different monitoring missions and shows current activity for a variety of sources.
		+
		+	See [[List of Be X-ray Binaries]] for details about individual sources.

← Older revision		Revision as of 15:43, 12 April 2018
Line 10:		Line 10:

	[http://integral.esac.esa.int/bexrbmonitor/webpage_oneplot.php The BeXRB Monitor] page collects data from different monitoring missions and shows current activity for a variety of sources.		[http://integral.esac.esa.int/bexrbmonitor/webpage_oneplot.php The BeXRB Monitor] page collects data from different monitoring missions and shows current activity for a variety of sources.
−
−	~~<references>~~
−	~~{{#lst:List of references\|Stella1986a}}~~
−	~~{{#lst:List of references\|Reig2011a}}~~
−	~~{{#lst:List of references\|Negueruela2001a}}~~
−	~~{{#lst:List of references\|Negueruela2001b}}~~
−	~~{{#lst:List of references\|Okazaki2001a}}~~
−	~~</references>~~

@@ Line 5: / Line 5: @@
 Be/X-ray binary systems form the majority of accreting X-ray pulsars. In these systems the optical companion is a giant star which besides a  fast low-density wind also show an equatorial disk or flattened envelope  in fast rotation. This disk shows up through [http://en.wikipedia.org/wiki/Balmer_lines Balmer emission lines] (see, e.g., [http://www.astrosurf.com/~buil/us/bestar.htm The spectroscopic Be stars Atlas]. The X-ray emitting object is usually a neutron star on an eccentric  orbit (e=0.1-0.9). For a recent review of Be/X-ray binaries see Reig et al. (2011)<ref name = "Reig2011a" />.
-Most Be/X-ray binaries show transient activity and only very weak emission outside outbursts. Stella et al. (1986)<ref name = "Stella1986" /> have classified the different outbursts in two types: Type I are periodical outbursts linked to the periastron passage of the neutron star and relatively short; Type II are larger outbursts with no clear link to the orbital phase.
+Most Be/X-ray binaries show transient activity and only very weak emission outside outbursts. Stella et al. (1986)<ref name = "Stella1986a" /> have classified the different outbursts in two types: Type I are periodical outbursts linked to the periastron passage of the neutron star and relatively short; Type II are larger outbursts with no clear link to the orbital phase.
-Historically, type I outbursts have been explained by a simple picture of the passage of the neutron star through the equatorial disk of the Be star every orbit. But this picture fails to explain the large variety of outbursts seen in many systems with periods of regular outbursts, occasional giant outbursts, but also extended periods of quiescence. A possible explanation was given by the [http://harmas.arc.hokkai-s-u.ac.jp/~okazaki/BeX/index.html model developed by Atsuo Okazaki] in which the disk around the Be star will often be truncated due to tidal interactions and outbursts are triggered by changes in the disk. This model has been published in Negueruela & Okazaki 2001<ref name = "Negueruela2001a" />, Negueruela (2001)<ref name = "Negueruela2001a" />, and Okazaki & Negueruela (2001)<ref name = "Okazaki2001a" />.
+Historically, type I outbursts have been explained by a simple picture of the passage of the neutron star through the equatorial disk of the Be star every orbit. But this picture fails to explain the large variety of outbursts seen in many systems with periods of regular outbursts, occasional giant outbursts, but also extended periods of quiescence. A possible explanation was given by the [http://harmas.arc.hokkai-s-u.ac.jp/~okazaki/BeX/index.html model developed by Atsuo Okazaki] in which the disk around the Be star will often be truncated due to tidal interactions and outbursts are triggered by changes in the disk. This model has been published in Negueruela & Okazaki 2001<ref name = "Negueruela2001a" />, Negueruela et al. (2001)<ref name = "Negueruela2001b" />, and Okazaki & Negueruela (2001)<ref name = "Okazaki2001a" />.
 [http://integral.esac.esa.int/bexrbmonitor/webpage_oneplot.php The BeXRB Monitor] page collects data from different monitoring missions and shows current activity for a variety of sources.