The outer evolution of instability-generated structure in radiatively driven stellar winds

By M. Runacres, S. Owocki. 2002

139 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Fluid Flow and Transfer Processes

View Paper: https://www.semanticscholar.org/paper/ec32cb819722bba9e67c7878c55438516d684cf4

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. N. Smith
2. N. Langer
3. F. Najarro
4. J. Vink
5. J. Puls
6. P. Crowther
7. D. John Hillier
8. Selma de Mink

In Computational Mechanics

1. L. Oskinova
2. A. Feldmeier
3. W. Hamann
4. P. Crowther
5. J. Puls
6. I. Brott
7. R. Genzel
8. A. ud-Doula

In Fluid Flow and Transfer Processes

1. W. Hamann
2. L. Oskinova
3. A. Feldmeier
4. J. Puls

Citations in the corpus

• Lower mass loss rates in O-type stars: Spectral signatures of dense clumps in the wind of two Galactic O4 stars (2004, background): “The location of the strongest clumping (expected to depend on the maximum line strength according to Runacres & Owocki (2002)) might then be in the region where Brγ forms.”
• The most massive stars in the Arches cluster (2007, result): “This is in agreement (qualitatively and quantitatively) with the recent findings of Puls et al. (2006) and with the theoretical predictions of Runacres & Owocki (2002).”
• Bright OB stars in the Galaxy. III. Constraints on the radial stratification of the clumping factor (2006, methodology): “Let us now compare our results with the predicted radial stratification of fcl itself (Runacres & Owocki 2002, 2005).”
• Chandra HETGS Multiphase Spectroscopy of the Young Magnetic O Star θ1 Orionis C (2005, methodology): “D simulations using a non-local, non-Sobolev formulation for the line-force (Owocki, Castor, & Rybicki 1988; Owocki & Puls 1999; Runacres & Owocki 2002) show this instability can lead to embedded weak shock structures that might reproduce the soft X-ray emission (Feldmeier 1995; Feldmeier, Puls, &…”
• Mass loss from hot massive stars (2008, background): “D “pseudo-periodic box formalism” to investigate the evolution at distances very far from the central star, Runacres and Owocki (2005, see also Runacres and Owocki 2002) showed that structure can survive out to distances of more than 1000 stellar radii, due to supersonic clump-clump collisions…”
• Neglecting the porosity of hot-star winds can lead to underestimating mass-loss rates (2007, methodology): “This assumption is corroborated by the hydrodynamical models (Feldmeier et al. 1997; Runacres & Owocki 2002; Dessart & Owocki 2005), that predict that the over-dense structures accelerate radially with 3(r) and, in general, do not split or merge.”
• Sub-surface convection zones in hot massive stars and their observable consequences (2009, result): “Apparently, this type of radial behavior is not consistent with hydrodynamical predictions of the intrinsic, self-excited linedriven instability (Runacres & Owocki 2002, 2005).”
• Physical parameters and wind properties of galactic early B supergiants (2005, background): “…clumping, if present,is predicted to affect these measurements in different ways – Hα samples the highest density region immediately above the photosphere, whilst the mid-IR continuum samples free-free emission , superimposed upon the stellar photosphere at larger radii (Runacres & Owocki 2002).”