On X-ray pulsations in β Cephei-type variables | Astronomy & Astrophysics (A&A)

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Volume 577 (May 2015)

A&A, 577 (2015) A32

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Table 1

XMM-Newton and Chandra observations of β Cep-variables covering at least three stellar pulsational periods.

	Sp	Period^a	Obs.	Counts^b	n _p ^c	X-ray period?	A _max ^d	Comment^e	Reference
		[h]

β Cen	B1III	3.684	XMM	25 000	6	no	<3%	mag	Raassen et al. (2005)
β Cep	B2IIIe	4.572	XMM	2500	9	no	<6%	mag	Favata et al. (2009)
β Cru	B0.5IV	4.589	CXO	225^f	4	no	< 26%^f	non-mag	this work
κ Sco	B1.5III	4.795	XMM	1700	3	no	<11%	?	this work
α Vir	B1.5IV-V	6.521	CXO	470	3	no	<21%	?	this work
ξ¹ CMa	B0.5-1IV	5.030	XMM	12 800	6	yes	10%	mag	Oskinova et al. (2014)

Notes.

^(a)

Main period of stellar oscillations as listed in the “Catalog of Galactic β Cephei stars” (Stankov & Handler 2005);

^(b)

number of counts per optical pulsation period (EPIC PN for XMM-Newton);

^(c)

number of pulsation periods covered by X-ray light curve;

^(d)

amplitude of X-ray pulsations or its upper limit for non-detections;

^(e)

magnetic field presence;

^(f)

in the hard band where the pulsations were suggested by Cohen et al. (2008).

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