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Accretion Processes in Mira AB

Published online by Cambridge University Press:  22 February 2018

M. Karovska ,
B. Wood ,
M. Marengo ,
J. C. Raymond ,
W. Hack  and
E. Guinan
M. Karovska
Affiliation:
Harvard-Smithsonian Astrophysical Observatory, CambridgeUSA
B. Wood
Affiliation:
JILA, BoulderUSA
M. Marengo
Affiliation:
Harvard-Smithsonian Astrophysical Observatory, CambridgeUSA
J. C. Raymond
Affiliation:
Harvard-Smithsonian Astrophysical Observatory, CambridgeUSA
W. Hack
Affiliation:
STScI, BaltimoreUSA
E. Guinan
Affiliation:
Villanova University, USA

Abstract

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The Mira AB interacting binary provides an ideal laboratory for studying mass loss and accretion processes in systems containing an AGB star and a compact accretor, because its components have been resolved and can be studied individually. We present here results from our long term study of accretion processes in this system. Those include recent HST observations suggesting that the accretion rate onto Mira B is much lower than before, indicating possible disruption of the accretion disk.

Resumen

Resumen

La binaria en interacción Mira AB representa un laboratorio ideal para estudiar la pérdida de masa y los procesos de acreción en sistemas que contienen una estrella AGB y una estrella acreciente compacta ya que sus componentes se resolvieron y pueden ser estudiados individualmente. Presentamos resultados de nuestro estudio de larga duración de procesos de acreción en este sistema, los cuales incluyen observaciones recientes del HST que sugieren que la tasa de acreción sobre Mira B es mucho menor que antes, lo cual indica una posible disrupción del disco de acreción.

Keywords

AccretionAccretion Disks — Stars: AGB and Post AGB — Stars: Mass Loss
Type
The Contributed Papers
Information
International Astronomical Union Colloquium , Volume 194: Compact binaries in the galaxy and beyond , 2004 , pp. 92 - 94
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

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