Changes in the red giant and dusty environment of the recurrent nova RS Ophiuchi following the 2006 eruption

M. T. Rushton; B. Kaminsky; D. K. Lynch; Ya V. Pavlenko; S. P S Eyres; C. E. Woodward; Ray W. Russell; Richard J. Rudy; Michael L. Sitko; T. Kerr; A. Evans

doi:10.1111/j.1365-2966.2009.15675.x

Changes in the red giant and dusty environment of the recurrent nova RS Ophiuchi following the 2006 eruption

M. T. Rushton, B. Kaminsky, D. K. Lynch, Ya V. Pavlenko, S. P S Eyres, C. E. Woodward, Ray W. Russell, Richard J. Rudy, Michael L. Sitko, T. Kerr, A. Evans

Cyfadran Cyfrifiadureg, Peirianneg a Gwyddoniaeth

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We present near-infrared spectroscopy of the recurrent nova RS Ophiuchi (RS Oph) obtained on several occasions after its latest outburst in 2006 February. The 1-5 μm spectra are dominated by the red giant, but the H i, He i and coronal lines present during the eruption are present in all our observations. From the fits of the computed infrared spectral energy distributions to the observed fluxes, we find T_eff = 4200 ± 200 K for the red giant. The first overtone CO bands at 2.3 μm, formed in the atmosphere of the red giant, are variable. The spectra clearly exhibit an infrared excess due to dust emission longward of 5 μm; we estimate an effective temperature for the emitting dust shell of 500 K, and find that the dust emission is also variable, being beyond the limit of detection in 2007. Most likely, the secondary star in RS Oph is intrinsically variable.

Iaith wreiddiol	Saesneg
Tudalennau (o-i)	99-104
Nifer y tudalennau	6
Cyfnodolyn	Monthly Notices of the Royal Astronomical Society
Cyfrol	401
Rhif cyhoeddi	1
Dynodwyr Gwrthrych Digidol (DOIs)	https://doi.org/10.1111/j.1365-2966.2009.15675.x
Statws	Cyhoeddwyd - Ion 2010

Mynediad at Ddogfen

10.1111/j.1365-2966.2009.15675.xTrwydded: CC BY-NC-ND

Dyfynnu hyn

Rushton, M. T., Kaminsky, B., Lynch, D. K., Pavlenko, Y. V., Eyres, S. P. S., Woodward, C. E., Russell, R. W., Rudy, R. J., Sitko, M. L., Kerr, T., & Evans, A. (2010). Changes in the red giant and dusty environment of the recurrent nova RS Ophiuchi following the 2006 eruption. Monthly Notices of the Royal Astronomical Society, 401(1), 99-104. https://doi.org/10.1111/j.1365-2966.2009.15675.x

@article{c935195213eb4da5972b79ada2a1b951,

title = "Changes in the red giant and dusty environment of the recurrent nova RS Ophiuchi following the 2006 eruption",

abstract = "We present near-infrared spectroscopy of the recurrent nova RS Ophiuchi (RS Oph) obtained on several occasions after its latest outburst in 2006 February. The 1-5 μm spectra are dominated by the red giant, but the H i, He i and coronal lines present during the eruption are present in all our observations. From the fits of the computed infrared spectral energy distributions to the observed fluxes, we find Teff = 4200 ± 200 K for the red giant. The first overtone CO bands at 2.3 μm, formed in the atmosphere of the red giant, are variable. The spectra clearly exhibit an infrared excess due to dust emission longward of 5 μm; we estimate an effective temperature for the emitting dust shell of 500 K, and find that the dust emission is also variable, being beyond the limit of detection in 2007. Most likely, the secondary star in RS Oph is intrinsically variable.",

keywords = "Binaries: symbiotic, Circumstellar matter, Infrared: stars, Novae, cataclysmic variables, Stars: individual: RS Ophiuchi",

author = "Rushton, {M. T.} and B. Kaminsky and Lynch, {D. K.} and Pavlenko, {Ya V.} and Eyres, {S. P S} and Woodward, {C. E.} and Russell, {Ray W.} and Rudy, {Richard J.} and Sitko, {Michael L.} and T. Kerr and A. Evans",

year = "2010",

month = jan,

doi = "10.1111/j.1365-2966.2009.15675.x",

language = "English",

volume = "401",

pages = "99--104",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "1",

}

Rushton, MT, Kaminsky, B, Lynch, DK, Pavlenko, YV, Eyres, SPS, Woodward, CE, Russell, RW, Rudy, RJ, Sitko, ML, Kerr, T & Evans, A 2010, 'Changes in the red giant and dusty environment of the recurrent nova RS Ophiuchi following the 2006 eruption', Monthly Notices of the Royal Astronomical Society, cyfrol. 401, rhif 1, tt. 99-104. https://doi.org/10.1111/j.1365-2966.2009.15675.x

TY - JOUR

T1 - Changes in the red giant and dusty environment of the recurrent nova RS Ophiuchi following the 2006 eruption

AU - Rushton, M. T.

AU - Kaminsky, B.

AU - Lynch, D. K.

AU - Pavlenko, Ya V.

AU - Eyres, S. P S

AU - Woodward, C. E.

AU - Russell, Ray W.

AU - Rudy, Richard J.

AU - Sitko, Michael L.

AU - Kerr, T.

AU - Evans, A.

PY - 2010/1

Y1 - 2010/1

N2 - We present near-infrared spectroscopy of the recurrent nova RS Ophiuchi (RS Oph) obtained on several occasions after its latest outburst in 2006 February. The 1-5 μm spectra are dominated by the red giant, but the H i, He i and coronal lines present during the eruption are present in all our observations. From the fits of the computed infrared spectral energy distributions to the observed fluxes, we find Teff = 4200 ± 200 K for the red giant. The first overtone CO bands at 2.3 μm, formed in the atmosphere of the red giant, are variable. The spectra clearly exhibit an infrared excess due to dust emission longward of 5 μm; we estimate an effective temperature for the emitting dust shell of 500 K, and find that the dust emission is also variable, being beyond the limit of detection in 2007. Most likely, the secondary star in RS Oph is intrinsically variable.

AB - We present near-infrared spectroscopy of the recurrent nova RS Ophiuchi (RS Oph) obtained on several occasions after its latest outburst in 2006 February. The 1-5 μm spectra are dominated by the red giant, but the H i, He i and coronal lines present during the eruption are present in all our observations. From the fits of the computed infrared spectral energy distributions to the observed fluxes, we find Teff = 4200 ± 200 K for the red giant. The first overtone CO bands at 2.3 μm, formed in the atmosphere of the red giant, are variable. The spectra clearly exhibit an infrared excess due to dust emission longward of 5 μm; we estimate an effective temperature for the emitting dust shell of 500 K, and find that the dust emission is also variable, being beyond the limit of detection in 2007. Most likely, the secondary star in RS Oph is intrinsically variable.

KW - Binaries: symbiotic

KW - Circumstellar matter

KW - Infrared: stars

KW - Novae, cataclysmic variables

KW - Stars: individual: RS Ophiuchi

U2 - 10.1111/j.1365-2966.2009.15675.x

DO - 10.1111/j.1365-2966.2009.15675.x

M3 - Article

AN - SCOPUS:72649094175

SN - 0035-8711

VL - 401

SP - 99

EP - 104

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

Changes in the red giant and dusty environment of the recurrent nova RS Ophiuchi following the 2006 eruption

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