Polarimetry and photometry of the new AM Herculis system RE J1844-741

J. Bailey; L. Ferrario; D.T. Wickramasinghe; D.A.H. Buckley; J. Hough

Polarimetry and photometry of the new AM Herculis system RE J1844-741

J. Bailey, L. Ferrario, D.T. Wickramasinghe, D.A.H. Buckley, J. Hough

Centre for Astrophysics Research (CAR)

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Abstract

The ROSAT Wide Field Camera extreme-ultraviolet (EUV) source RE J1844-741 was identified with a 16th-magnitude cataclysmic variable with a period of 90 min by O'Donoghue et al. In this paper, we present spectropolarimetry and broad-band photometry and polarimetry of RE J1844-741 that confirm it to be a new, short-period, AM Herculis system. Our modelling of the circular polarization and light intensity curves in the 3400-4800 and 5500-8400 A bands indicates the presence of two linearly extended cyclotron emission regions on the surface of the white dwarf. The main emission region is located below the orbital plane, and it is visible for about 40 per cent of the orbital period. The secondary emission region is located above the orbital plane, is visible for approximately 60 per cent of the orbital period, and is responsible for the negatively circularly polarized intensity maxima which dominate the light curve during high states of activity.

Original language	English
Pages (from-to)	579-584
Journal	Monthly Notices of the Royal Astronomical Society (MNRAS)
Volume	272
Issue number	3
Publication status	Published - 1995

Keywords

accretion disks
cataclysmic variables
cyclotron emission

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@article{72d42e4802554929bbdb3b141936c387,

title = "Polarimetry and photometry of the new AM Herculis system RE J1844-741",

abstract = "The ROSAT Wide Field Camera extreme-ultraviolet (EUV) source RE J1844-741 was identified with a 16th-magnitude cataclysmic variable with a period of 90 min by O'Donoghue et al. In this paper, we present spectropolarimetry and broad-band photometry and polarimetry of RE J1844-741 that confirm it to be a new, short-period, AM Herculis system. Our modelling of the circular polarization and light intensity curves in the 3400-4800 and 5500-8400 A bands indicates the presence of two linearly extended cyclotron emission regions on the surface of the white dwarf. The main emission region is located below the orbital plane, and it is visible for about 40 per cent of the orbital period. The secondary emission region is located above the orbital plane, is visible for approximately 60 per cent of the orbital period, and is responsible for the negatively circularly polarized intensity maxima which dominate the light curve during high states of activity.",

keywords = "accretion disks, cataclysmic variables, cyclotron emission",

author = "J. Bailey and L. Ferrario and D.T. Wickramasinghe and D.A.H. Buckley and J. Hough",

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 = "1995",

language = "English",

volume = "272",

pages = "579--584",

journal = "Monthly Notices of the Royal Astronomical Society (MNRAS)",

issn = "0035-8711",

publisher = "Oxford University Press (OUP)",

number = "3",

}

TY - JOUR

T1 - Polarimetry and photometry of the new AM Herculis system RE J1844-741

AU - Bailey, J.

AU - Ferrario, L.

AU - Wickramasinghe, D.T.

AU - Buckley, D.A.H.

AU - Hough, J.

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 - 1995

Y1 - 1995

N2 - The ROSAT Wide Field Camera extreme-ultraviolet (EUV) source RE J1844-741 was identified with a 16th-magnitude cataclysmic variable with a period of 90 min by O'Donoghue et al. In this paper, we present spectropolarimetry and broad-band photometry and polarimetry of RE J1844-741 that confirm it to be a new, short-period, AM Herculis system. Our modelling of the circular polarization and light intensity curves in the 3400-4800 and 5500-8400 A bands indicates the presence of two linearly extended cyclotron emission regions on the surface of the white dwarf. The main emission region is located below the orbital plane, and it is visible for about 40 per cent of the orbital period. The secondary emission region is located above the orbital plane, is visible for approximately 60 per cent of the orbital period, and is responsible for the negatively circularly polarized intensity maxima which dominate the light curve during high states of activity.

AB - The ROSAT Wide Field Camera extreme-ultraviolet (EUV) source RE J1844-741 was identified with a 16th-magnitude cataclysmic variable with a period of 90 min by O'Donoghue et al. In this paper, we present spectropolarimetry and broad-band photometry and polarimetry of RE J1844-741 that confirm it to be a new, short-period, AM Herculis system. Our modelling of the circular polarization and light intensity curves in the 3400-4800 and 5500-8400 A bands indicates the presence of two linearly extended cyclotron emission regions on the surface of the white dwarf. The main emission region is located below the orbital plane, and it is visible for about 40 per cent of the orbital period. The secondary emission region is located above the orbital plane, is visible for approximately 60 per cent of the orbital period, and is responsible for the negatively circularly polarized intensity maxima which dominate the light curve during high states of activity.

KW - accretion disks

KW - cataclysmic variables

KW - cyclotron emission

M3 - Article

SN - 0035-8711

VL - 272

SP - 579

EP - 584

JO - Monthly Notices of the Royal Astronomical Society (MNRAS)

JF - Monthly Notices of the Royal Astronomical Society (MNRAS)

IS - 3

ER -

Polarimetry and photometry of the new AM Herculis system RE J1844-741

Abstract

Keywords

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