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Chandra X-Ray Results on V426 Ophiuchi

Published online by Cambridge University Press:  22 February 2018

Lee Homer ,
Paula Szkody ,
John C. Raymond ,
Robert E. Fried ,
D. W. Hoard ,
S. L. Hawley ,
M. Wolfe ,
J. N. Tramposch  and
K. Т. Yirak
Lee Homer
Affiliation:
Astronomy Department, Box 351580, University of Washington, Seattle, WA 98195-1580 (homer@astro.Washington.edu)
Paula Szkody
Affiliation:
Astronomy Department, Box 351580, University of Washington, Seattle, WA 98195-1580 (homer@astro.Washington.edu)
John C. Raymond
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA 02138
Robert E. Fried
Affiliation:
Braeside Observatory, P. O. Box 906, Flagstaff, AZ 86002
D. W. Hoard
Affiliation:
SIRTF Science Center, California Institute of Technology, 1200 E. California Blvd, Pasadena, СA 91125
S. L. Hawley
Affiliation:
Astronomy Department, Box 351580, University of Washington, Seattle, WA 98195-1580 (homer@astro.Washington.edu)
M. Wolfe
Affiliation:
Astronomy Department, Box 351580, University of Washington, Seattle, WA 98195-1580 (homer@astro.Washington.edu)
J. N. Tramposch
Affiliation:
Astronomy Department, Box 351580, University of Washington, Seattle, WA 98195-1580 (homer@astro.Washington.edu)
K. Т. Yirak
Affiliation:
Astronomy Department, Box 351580, University of Washington, Seattle, WA 98195-1580 (homer@astro.Washington.edu)

Abstract

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From a 45ks Chandra observation of V42G Oph we have obtained high-resolution X-ray spectra at moderate signal-to-noise, and a, good quality, uninterrupted lightcurve. The spectra are reasonably fit with a cooling flow model, similar to EX Hya and U Gem. Our analysis of the Chandra and additional X-ray/optical lightcurves reveals a persistent modulation at 4.2 hr from 1988 to 2003, likely the white dwarf spin period indicating an intermediate polar nature for V426 Oph.

Resumen

Resumen

De las observaciones de 45 ks de Chandra de V42G Oph hemos obtenido espectros de rayos X de alta resolución con relación señal-a-ruido moderada, y una curva de luz no interrumpida de buena calidad. Los espectros se adaptan razonablemente a un modelo de flujo de enfriamiento, similar a EX Hya y U Gem. Nuestro análisis de las curvas de luz de Chandra y las adicionales de rayos X/óptico revela una modulación persistente a 4.2 hr desde 1988 hasta 2003, probablemente el período de giro de la enana blanca, indicando una naturaleza polar intermedia, para, V426 Oph.

Keywords

AccretionAccretion Disks — StarsIndividual (V426 Ophiuchi)
Type
The Contributed Papers
Information
International Astronomical Union Colloquium , Volume 194: Compact binaries in the galaxy and beyond , 2004 , pp. 176 - 177
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

References

Hellier, C. et al., MNRAS, 242, 32P Google Scholar
Herbig, G. H. 1960, ApJ, 131, 632 Google Scholar
Hessman, F. V. 1988, A&AS, 72, 515 Google Scholar
King, A. R. & Wynn, G. A. 1999, MNRAS, 310, 203 CrossRefGoogle Scholar
Mukai, K. et al. 2003 ApJ, 586, L77 CrossRefGoogle Scholar
Norton, A. J. et al. 2003 ASP C. Ser., (astro-ph/0301351)Google Scholar
Raymond, J. C. 1979, ApJS, 39, 1 Google Scholar
Rosen, S. R. et al. 1994, MNRAS, 269, 913 Google Scholar
Scargle, J. D. 1982, ApJ, 263, 835 Google Scholar
Stellingwerf, R. F. 1978, ApJ, 224, 953 Google Scholar
Szkody, P. 1986, ApJ, 301, L29 Google Scholar
Szkody, P., Kii, T., & Osaki, Y. 1990, AJ, 100, 546 Google Scholar