Stellar Wind Signatures in sdB Stars

U. Heber; P.F.L. Maxted; T.R. Marsh; C. Knigge; J.E. Drew

Stellar Wind Signatures in sdB Stars

U. Heber, P.F.L. Maxted, T.R. Marsh, C. Knigge, J.E. Drew

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Abstract

Subdwarf B (sdB) stars form the blue end of the horizontal branch. Their peculiar atmospheric-abundance patters result from diffusion processes. However, diffusion models fail to explain these anomalies quantitatively. From a NLTE model-atmosphere analysis of 40 sdB stars, we found that the more luminous (i.e. more evolved) stars have anomalous Ha and He I6678A line profiles, i.e. the lines are too broad and shallow, and may even show some emission. We interpret these anomalies as the signatures of a stellar wind, the first such detection in this class of star (if confirmed). Mass-loss may also explain the peculiar abundance patterns see in sdB stars. High-quality UV spectra are needed to confirm that these stars do have stellar winds.

Original language	English
Title of host publication	In: Procs of Stellar Atmosphere Modeling, ASP Conference Proceedings 288
Publisher	Astronomical Society of the Pacific
Pages	251-4
ISBN (Print)	1-58381-131-1
Publication status	Published - 2003

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title = "Stellar Wind Signatures in sdB Stars",

abstract = "Subdwarf B (sdB) stars form the blue end of the horizontal branch. Their peculiar atmospheric-abundance patters result from diffusion processes. However, diffusion models fail to explain these anomalies quantitatively. From a NLTE model-atmosphere analysis of 40 sdB stars, we found that the more luminous (i.e. more evolved) stars have anomalous Ha and He I6678A line profiles, i.e. the lines are too broad and shallow, and may even show some emission. We interpret these anomalies as the signatures of a stellar wind, the first such detection in this class of star (if confirmed). Mass-loss may also explain the peculiar abundance patterns see in sdB stars. High-quality UV spectra are needed to confirm that these stars do have stellar winds.",

author = "U. Heber and P.F.L. Maxted and T.R. Marsh and C. Knigge and J.E. Drew",

note = "Original paper can be found at: http://www.astrosociety.org/pubs/cs/286.html--Copyright Astronomical Society of the Pacific",

year = "2003",

language = "English",

isbn = "1-58381-131-1",

pages = "251--4",

booktitle = "In: Procs of Stellar Atmosphere Modeling, ASP Conference Proceedings 288",

publisher = "Astronomical Society of the Pacific",

address = "United States",

}

TY - GEN

T1 - Stellar Wind Signatures in sdB Stars

AU - Heber, U.

AU - Maxted, P.F.L.

AU - Marsh, T.R.

AU - Knigge, C.

AU - Drew, J.E.

N1 - Original paper can be found at: http://www.astrosociety.org/pubs/cs/286.html--Copyright Astronomical Society of the Pacific

PY - 2003

Y1 - 2003

N2 - Subdwarf B (sdB) stars form the blue end of the horizontal branch. Their peculiar atmospheric-abundance patters result from diffusion processes. However, diffusion models fail to explain these anomalies quantitatively. From a NLTE model-atmosphere analysis of 40 sdB stars, we found that the more luminous (i.e. more evolved) stars have anomalous Ha and He I6678A line profiles, i.e. the lines are too broad and shallow, and may even show some emission. We interpret these anomalies as the signatures of a stellar wind, the first such detection in this class of star (if confirmed). Mass-loss may also explain the peculiar abundance patterns see in sdB stars. High-quality UV spectra are needed to confirm that these stars do have stellar winds.

AB - Subdwarf B (sdB) stars form the blue end of the horizontal branch. Their peculiar atmospheric-abundance patters result from diffusion processes. However, diffusion models fail to explain these anomalies quantitatively. From a NLTE model-atmosphere analysis of 40 sdB stars, we found that the more luminous (i.e. more evolved) stars have anomalous Ha and He I6678A line profiles, i.e. the lines are too broad and shallow, and may even show some emission. We interpret these anomalies as the signatures of a stellar wind, the first such detection in this class of star (if confirmed). Mass-loss may also explain the peculiar abundance patterns see in sdB stars. High-quality UV spectra are needed to confirm that these stars do have stellar winds.

M3 - Conference contribution

SN - 1-58381-131-1

SP - 251

EP - 254

BT - In: Procs of Stellar Atmosphere Modeling, ASP Conference Proceedings 288

PB - Astronomical Society of the Pacific

ER -

Stellar Wind Signatures in sdB Stars

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