Mass Loss by Hot Stars

Lucy, L. B.; Solomon, P. M.

doi:10.1086/150365

Cited by 552 publications

(368 citation statements)

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“…The investigations were continued with ASCA (Corcoran et al 1994) and ROSAT (Haberl & White 1993;Berghöfer et al 1996). Although the origin of the emission was initially a matter of debate, it is now generally believed that instabilities and clumping in the strong line-driven stellar wind is the mechanism that heats small parts of the wind (e.g., Lucy & Solomon 1970;Lucy & White 1980;Lucy 1982;Owocki et al 1988;Dessart & Owocki 2005). The launches of Chandra and XMM-Newton in 1999 with high-resolution instruments aboard have offered the possibility to study the X-ray spectra in more detail, resulting in, e.g., estimates of line ratios, line profiles, temperatures, emission measures, and abundances (Waldron & Cassinelli 2001Cohen et al 2006;Kahn et al 2001;Raassen et al 2008).…”

Section: Introductionmentioning

confidence: 99%

The X-ray spectrum ofδOrionis observed by LETGS aboardChandra

Raassen

Pollock

2013

A&A

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Aims. We analyze the high-resolution X-ray spectrum of the supergiant O-star δ Orionis (O9.5II) with line ratios of He-like ions and a thermal plasma model, and we examine its variability. Methods. The O-supergiant δ Ori was observed in the wavelength range 5-175 Å by the X-ray detector HRC-S in combination with the grating LETG aboard Chandra. We studied the He-like ions in combination with the UV-radiation field to determine local plasma temperatures and to establish the distance of the X-ray emitting ions to the stellar surface. We measured individual lines by means of Gaussian profiles, folded through the response matrix, to obtain wavelengths, line fluxes, half widths at half maximum (HWHM) and line shifts to characterize the plasma. We consider multitemperature models in collisional ionization equilibrium (CIE) to determine temperatures, emission measures, and abundances.Results. Analysis of the He-like triplets extended to N vi and C v implies ionization stratification with the hottest plasma to be found within a few stellar radii 3 R * (Mg xi) and the coolest farther out, far beyond the acceleration zone, up to 49 R * (N vi) and 75 R * (C v).The observed temperatures cover a range from about 0.1 to 0.7 keV, i.e., 1-8 MK. The X-ray luminosity (L x ) is ∼1.5 × 10 32 erg/s in the range from 0.07 to 3 keV covered by LETGS. Velocity widths of about 1040 km s −1 have been determined.

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Section: Introductionmentioning

confidence: 99%

The X-ray spectrum ofδOrionis observed by LETGS aboardChandra

Raassen

Pollock

2013

A&A

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“…Small-scale structures are explained by reverse shocks in the wind, which are caused by a very strong, intrinsic instability in line-drive winds (LDI), already noted by Lucy & Solomon (1970). Numerical hydrodynamical modelling, e.g., by Feldmeier (1995) or Sundqvist & Owocki (2013) finds that the wind plasma becomes compressed into spatially narrow "clumps" separated by large regions of rarefied gas.…”

Section: Structures In Winds From Massive Starsmentioning

confidence: 97%

Stellar Winds in Massive X-ray Binaries

Kretschmar¹,

Martínez-Núñez

Bozzo

et al. 2016

Proc. IAU

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Abstract. Strong winds from massive stars are a topic of interest to a wide range of astrophysical fields. In High-Mass X-ray Binaries the presence of an accreting compact object on the one side allows to infer wind parameters from studies of the varying properties of the emitted X-rays; but on the other side the accretor's gravity and ionizing radiation can strongly influence the wind flow. Based on a collaborative effort of astronomers both from the stellar wind and the X-ray community, this presentation attempts to review our current state of knowledge and indicate avenues for future progress.

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“…Radiation pressure as a driving mechanism for stellar outflow was rediscovered by Lucy and Solomon (1970) who developed the basis of the theory and the first attempt to its solution. The pioneering step in the formulation of the theory in a quasi self-consistent manner was performed by Castor, Abbott, and Klein (1975).…”

Section: Concept For Consistent Models Of Hot Star Atmospheresmentioning

confidence: 99%

Hot Stars: Old-Fashioned or Trendy?

Pauldrach¹

Reviews in Modern Astronomy 16

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Mass Loss by Hot Stars

Cited by 552 publications

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The X-ray spectrum ofδOrionis observed by LETGS aboardChandra

The X-ray spectrum ofδOrionis observed by LETGS aboardChandra

Stellar Winds in Massive X-ray Binaries

Hot Stars: Old-Fashioned or Trendy?

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