Analysis of the photometric variability of WR40⋆

Gosset, Éric; Vreux, Jean-Marie; Manfroid, Jean; Sterken, C.; Walker, E. N.; Haefner, R.

doi:10.1093/mnras/238.1.97

Cited by 12 publications

(11 citation statements)

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“…In the season g a new automatic photometer was installed at the telescope, with a rather different V passband. Gosset et al (1991). HD 93695: NSV 4978, but our data do not show any variability.…”

Section: Observationscontrasting

confidence: 60%

Sixty four nights of UBV photometry of early‐type stars at La Sila

Mayer¹,

Božić

Lorenz³

et al. 2010

Astron Nachr

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UBV measurements of early-type stars, mostly eclipsing binaries, obtained at La Silla in the years 1990 to 1994 with the ESO 50 cm telescope are presented. Most of these data were already used in our individual studies of several binaries. Now all photometric measurements were reduced again with an advanced technique and are made available electronically. Our data for MY Ser have not yet been published; new light curve is given and solved. The result is that MY Ser is a contact binary, with very large fill-out parameter. Also a light curve and its solution for V1051 Cen are provided, and the problem of the period of V871 Cen is pointed out. Besides binaries (and the comparison and check stars) data for several stars in southern H II regions are included. Extinction and transformation coefficients are given.

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Section: Observationscontrasting

confidence: 60%

Sixty four nights of UBV photometry of early‐type stars at La Sila

Mayer¹,

Božić

Lorenz³

et al. 2010

Astron Nachr

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“…All periodicities emerging from photometry, spectroscopy or polarimetry are completely inconsistent, with strong epoch dependency and hints of multiperiodicities. As the best and most 'robust' examples of multiperiodic variability confirmed by numerous independent observations, we mention WR 16 (Gosset et al 1990;Antokhin et al 1995) and WR 40 Antokhin et al 1995). The only promising cases (besides the very longperiod visual binary WR 147) for a binary-like behaviour are WR 40, 66 and 124 (the last being the weakest).…”

Section: What Makes the Wn8 Stars So Violent?mentioning

confidence: 78%

A comprehensive variability study of the enigmatic WN8 stars: final results

Марченко

Moffat

Eversberg

et al. 1998

Monthly Notices of the Royal Astronomical Society

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A B S T R A C TAs a conclusion of our all-sky variability survey of the 'enigmatic' variable WN8 stars, we have carried out coordinated multisite photometric and spectroscopic observations of WN8 stars in 1989 and 1994-1995. We confirm the leading role of the stellar core in restructuring the whole wind. This emerges as a statistical trend: the higher the level of the #continuum (i.e. #core) light variations, the higher the variability of the P Cygni edges of the optical emission lines. However, the form of the correlation between the light and profile variations is generally different for each individual star. The high level of activity of WN8 stars may be supported/induced by pulsational instability.

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“…With a peak to peak amplitude of 0.1 mag, it is also one of the photometrically most variable ones (Lamontagne & Moffat 1987). The debate on the presence of deterministic variations in the photometry is, in our opinion, still open (Smith et al 1985;Gosset et al 1989;Balona et al 1989;Gosset & Vreux 1990;Matthews & Moffat 1994;Antokhin et al 1995;Marchenko et al 1998). Although WR 40 is considered to be a single star, its spectrum is extremely complex as well as strongly variable (see a first study by Moffat & Isserstedt 1980).…”

Section: Characteristics Of Wr 40mentioning

confidence: 99%

AnXMM-Newtonlook at the Wolf-Rayet star WR 40

Gosset¹,

Nazé²,

Claeskens³

et al. 2004

A&A

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Abstract. We present the results of an XMM-Newton observation of the field of the Wolf-Rayet star WR 40. Despite a nominal exposure of 20 ks and the high sensitivity of the satellite, the star itself is not detected: we thus derive an upper limit on its X-ray flux and luminosity. Joining this result to recent reports of a non-detection of some WC stars, we suggest that the X-ray emission from single normal Wolf-Rayet stars could often be insignificant despite remarkable instabilities in the wind. On the basis of a simple modelling of the opacity of the Wolf-Rayet wind of WR 40, we show that any X-ray emission generated in the particular zone where the shocks are supposed to be numerous will indeed have little chance to emerge from the dense wind of the Wolf-Rayet star. We also report the non-detection of the ejecta nebula RCW 58 surrounding WR 40. Concerning the field around these objects, we detected 33 X-ray sources, most of them previously unknown: we establish a catalog of these sources and cross-correlate it with catalogs of optical/infrared sources.

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Analysis of the photometric variability of WR40⋆

Cited by 12 publications

References 0 publications

Sixty four nights of UBV photometry of early‐type stars at La Sila

Sixty four nights of UBV photometry of early‐type stars at La Sila

A comprehensive variability study of the enigmatic WN8 stars: final results

AnXMM-Newtonlook at the Wolf-Rayet star WR 40

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