An optical and near-infrared study of the AM Herculis-type binary CW 1103+254

J. Bailey; D.J. Watts; M.R. Sherrington; D.J. Axon; A.B. Giles; D.A. Hanes; S.R. Heathcote; J. Hough; S. Hughes; R.F. Jameson; I. McLean

An optical and near-infrared study of the AM Herculis-type binary CW 1103+254

J. Bailey, D.J. Watts, M.R. Sherrington, D.J. Axon, A.B. Giles, D.A. Hanes, S.R. Heathcote, J. Hough, S. Hughes, R.F. Jameson, I. McLean

Centre for Astrophysics Research (CAR)

Research output: Contribution to journal › Article › peer-review

Abstract

All main components of the AM Herculis-type binary CW 1103 + 254 can be distinguished by means of observations encompassing optical and near-IR photometry and polarimetry, together with optical spectroscopy and spectropolarimetry. The M-dwarf secondary's IR magnitude is used to estimate the distance of the system as 136 pc. Observed emission line profiles can be understood in terms of two components, one of which originates in the white dwarf's infalling stream of material while the other comes from the vicinity of the secondary. The excess radiation noted during the bright phase can be understood as cyclotron radiation from the shock-heated region near the white dwarf magnetic pole. Changes that occurred in the system in 1982 and 1983 indicate precessional motion of either the white dwarf rotation or the magnetic axis.

Original language	English
Pages (from-to)	179-196
Journal	Monthly Notices of the Royal Astronomical Society
Volume	215
Issue number	2
Publication status	Published - 1985

Cite this

@article{19d80a93a1544729b31e79facc1e46f6,

title = "An optical and near-infrared study of the AM Herculis-type binary CW 1103+254",

abstract = "All main components of the AM Herculis-type binary CW 1103 + 254 can be distinguished by means of observations encompassing optical and near-IR photometry and polarimetry, together with optical spectroscopy and spectropolarimetry. The M-dwarf secondary's IR magnitude is used to estimate the distance of the system as 136 pc. Observed emission line profiles can be understood in terms of two components, one of which originates in the white dwarf's infalling stream of material while the other comes from the vicinity of the secondary. The excess radiation noted during the bright phase can be understood as cyclotron radiation from the shock-heated region near the white dwarf magnetic pole. Changes that occurred in the system in 1982 and 1983 indicate precessional motion of either the white dwarf rotation or the magnetic axis.",

author = "J. Bailey and D.J. Watts and M.R. Sherrington and D.J. Axon and A.B. Giles and D.A. Hanes and S.R. Heathcote and J. Hough and S. Hughes and R.F. Jameson and I. McLean",

note = "Original article can be found via: http://cdsads.u-strasbg.fr/ Copyright Royal Astronomical Society [Full text of this article is not available in the UHRA]",

year = "1985",

language = "English",

volume = "215",

pages = "179--196",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press (OUP)",

number = "2",

}

TY - JOUR

T1 - An optical and near-infrared study of the AM Herculis-type binary CW 1103+254

AU - Bailey, J.

AU - Watts, D.J.

AU - Sherrington, M.R.

AU - Axon, D.J.

AU - Giles, A.B.

AU - Hanes, D.A.

AU - Heathcote, S.R.

AU - Hough, J.

AU - Hughes, S.

AU - Jameson, R.F.

AU - McLean, I.

N1 - Original article can be found via: http://cdsads.u-strasbg.fr/ Copyright Royal Astronomical Society [Full text of this article is not available in the UHRA]

PY - 1985

Y1 - 1985

N2 - All main components of the AM Herculis-type binary CW 1103 + 254 can be distinguished by means of observations encompassing optical and near-IR photometry and polarimetry, together with optical spectroscopy and spectropolarimetry. The M-dwarf secondary's IR magnitude is used to estimate the distance of the system as 136 pc. Observed emission line profiles can be understood in terms of two components, one of which originates in the white dwarf's infalling stream of material while the other comes from the vicinity of the secondary. The excess radiation noted during the bright phase can be understood as cyclotron radiation from the shock-heated region near the white dwarf magnetic pole. Changes that occurred in the system in 1982 and 1983 indicate precessional motion of either the white dwarf rotation or the magnetic axis.

AB - All main components of the AM Herculis-type binary CW 1103 + 254 can be distinguished by means of observations encompassing optical and near-IR photometry and polarimetry, together with optical spectroscopy and spectropolarimetry. The M-dwarf secondary's IR magnitude is used to estimate the distance of the system as 136 pc. Observed emission line profiles can be understood in terms of two components, one of which originates in the white dwarf's infalling stream of material while the other comes from the vicinity of the secondary. The excess radiation noted during the bright phase can be understood as cyclotron radiation from the shock-heated region near the white dwarf magnetic pole. Changes that occurred in the system in 1982 and 1983 indicate precessional motion of either the white dwarf rotation or the magnetic axis.

M3 - Article

SN - 0035-8711

VL - 215

SP - 179

EP - 196

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

An optical and near-infrared study of the AM Herculis-type binary CW 1103+254

Abstract

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