2015A&A...580A..59R


C.D.S. - SIMBAD4 rel 1.7 - 2020.02.17CET02:52:46

2015A&A...580A..59R - Astronomy and Astrophysics, volume 580A, 59-59 (2015/8-1)

Simultaneous X-ray and optical spectroscopy of the Oef supergiant λ Cephei.

RAUW G., HERVE A., NAZE Y., GONZALEZ-PEREZ J.N., HEMPELMANN A., MITTAG M., SCHMITT J.H.M.M., SCHROEDER K.-P., GOSSET E., EENENS P. and UUH-SONDA J.M.

Abstract (from CDS):

Probing the structures of stellar winds is of prime importance for the understanding of massive stars. Based on their optical spectral morphology and variability, it has been suggested that the stars in the Oef class feature large-scale structures in their wind. High-resolution X-ray spectroscopy and time-series of X-ray observations of presumably single O-type stars can help us understand the physics of their stellar winds. We have collected XMM-Newton observations and coordinated optical spectroscopy of the O6Ief star λ Cep to study its X-ray and optical variability and to analyse its high-resolution X-ray spectrum. We investigate the line profile variability of the HeII λ4686 and Hα emission lines in our time series of optical spectra, including a search for periodicities. We further discuss the variability of the broadband X-ray flux and analyse the high-resolution spectrum of λ Cep using line-by-line fits as well as a code designed to fit the full high-resolution X-ray spectrum consistently. During our observing campaign, the HeII λ4686 line varies on a timescale of ∼18h. On the contrary, the Hα line profile displays a modulation on a timescale of 4.1days which is likely the rotation period of the star. The X-ray flux varies on timescales of days and could in fact be modulated by the same 4.1-day period as Hα, although both variations are shifted in phase. The high-resolution X-ray spectrum reveals broad and skewed emission lines as expected for the X-ray emission from a distribution of wind-embedded shocks. Most of the X-ray emission arises within less than 2R* above the photosphere. The properties of the X-ray emission of λ Cep generally agree with the expectations of the wind-embedded shock model. There is mounting evidence for the existence of large-scale structures that modulate the Hα line and about 10% of the X-ray emission of λ Cep.

Abstract Copyright:

Journal keyword(s): stars: early-type - stars: massive - stars: individual: λ Cep - X-rays: stars

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * ksi Per ** 03 58 57.9022917 +35 47 27.713205 3.190 4.080 4.060 3.88 3.89 O7.5III(n)((f)) 788 0
2 * del Ori Al* 05 32 00.40009 -00 17 56.7424 0.96 2.02 2.41 2.32 2.54 B0III+O9V 741 0
3 * tet01 Ori C ** 05 35 16.46375 -05 23 22.8486 4.20 5.15 5.13 4.91 4.73 O7Vp 1264 1
4 * ksi01 CMa bC* 06 31 51.3663578 -23 25 06.318090 3.10 4.09 4.33 4.45 4.72 B0.7IV 295 0
5 * J Pup * 07 53 18.1579197 -48 06 10.563676 3.11 4.10 4.24 4.26 4.38 B0.5Ib 218 0
6 * zet Pup BY* 08 03 35.04754 -40 00 11.3321 0.89 1.98 2.25 2.36 2.58 O4I(n)fp 1087 1
7 HD 93521 * 10 48 23.5116139485 +37 34 13.089937784 5.67 6.79 7.03     O9.5IIInn 399 1
8 HD 148937 SB* 16 33 52.3867163783 -48 06 40.476619334 6.49 7.12 6.71 7.61   O6f?p 351 4
9 * zet Oph Be* 16 37 09.5390545 -10 34 01.529471 1.73 2.58 2.56 2.46 2.50 O9.2IVnn 1717 2
10 * lam Cep s*b 22 11 30.5750839949 +59 24 52.147736074 4.55 5.29 5.05 4.77 4.62 O6.5I(n)fp 644 1

    Equat.    Gal    SGal    Ecl

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2020.02.17-02:52:46

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