High-resolution x-ray spectroscopy of the evolving shock in the 2006 outburst of RS Ophiuchi

J. U. Ness, J. J. Drake, Sumner Starrfield, M. F. Bode, T. J. O'Brien, A. Evans, S. P S Eyres, L. A. Helton, J. P. Osborne, K. L. Page, C. Schneider, C. E. Woodward

Research output: Contribution to journalArticle

33 Citations (Scopus)

Abstract

The evolution of the 2006 outburst of the recurrent nova RSOphiuchi was followed with 12 X-ray grating observations with Chandra and XMM-Newton. We present detailed spectral analyses using two independent approaches. From the best data set, taken on day 13.8 after outburst, we reconstruct the temperature distribution and derive elemental abundances. We find evidence for at least two distinct temperature components on day 13.8 and a reduction of temperature with time. The X-ray flux decreases as a power law, and the power-law index changes from -5/3 to -8/3 around day 70 after outburst. This can be explained by different decay mechanisms for the hot and cool components. The decay of the hot component and the decrease in temperature are consistent with radiative cooling, while the decay of the cool component can be explained by the expansion of the ejecta. We find overabundances of N and of α elements, which could either represent the composition of the secondary that provides the accreted material or that of the ejecta. The N overabundance indicates CNO-cycled material. From comparisons to abundances for the secondary taken from the literature, we conclude that 20%-40% of the observed nitrogen could originate from the outburst. The overabundance of the α elements is not typical for stars of the spectral type of the secondary in the RSOph system, and white dwarf material might have been mixed into the ejecta. However, no direct measurements of the α elements in the secondary are available, and the continuous accretion may have changed the observable surface composition.

Original languageEnglish (US)
Pages (from-to)3414-3436
Number of pages23
JournalAstronomical Journal
Volume137
Issue number2
DOIs
StatePublished - 2009

Fingerprint

outburst
x ray spectroscopy
ejecta
shock
spectroscopy
high resolution
power law
decay
temperature
XMM-Newton telescope
newton
temperature distribution
x rays
accretion
gratings
cooling
nitrogen
stars
expansion
material

Keywords

  • Binaries: symbiotic
  • Methods: data analysis
  • Novae, cataclysmic variables
  • Shock waves
  • Stars: individual (RSOph)
  • X-rays: stars

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Ness, J. U., Drake, J. J., Starrfield, S., Bode, M. F., O'Brien, T. J., Evans, A., ... Woodward, C. E. (2009). High-resolution x-ray spectroscopy of the evolving shock in the 2006 outburst of RS Ophiuchi. Astronomical Journal, 137(2), 3414-3436. https://doi.org/10.1088/0004-6256/137/2/3414

High-resolution x-ray spectroscopy of the evolving shock in the 2006 outburst of RS Ophiuchi. / Ness, J. U.; Drake, J. J.; Starrfield, Sumner; Bode, M. F.; O'Brien, T. J.; Evans, A.; Eyres, S. P S; Helton, L. A.; Osborne, J. P.; Page, K. L.; Schneider, C.; Woodward, C. E.

In: Astronomical Journal, Vol. 137, No. 2, 2009, p. 3414-3436.

Research output: Contribution to journalArticle

Ness, JU, Drake, JJ, Starrfield, S, Bode, MF, O'Brien, TJ, Evans, A, Eyres, SPS, Helton, LA, Osborne, JP, Page, KL, Schneider, C & Woodward, CE 2009, 'High-resolution x-ray spectroscopy of the evolving shock in the 2006 outburst of RS Ophiuchi', Astronomical Journal, vol. 137, no. 2, pp. 3414-3436. https://doi.org/10.1088/0004-6256/137/2/3414
Ness, J. U. ; Drake, J. J. ; Starrfield, Sumner ; Bode, M. F. ; O'Brien, T. J. ; Evans, A. ; Eyres, S. P S ; Helton, L. A. ; Osborne, J. P. ; Page, K. L. ; Schneider, C. ; Woodward, C. E. / High-resolution x-ray spectroscopy of the evolving shock in the 2006 outburst of RS Ophiuchi. In: Astronomical Journal. 2009 ; Vol. 137, No. 2. pp. 3414-3436.
@article{0cb80e2cdf8640f3b26556c4329c28cd,
title = "High-resolution x-ray spectroscopy of the evolving shock in the 2006 outburst of RS Ophiuchi",
abstract = "The evolution of the 2006 outburst of the recurrent nova RSOphiuchi was followed with 12 X-ray grating observations with Chandra and XMM-Newton. We present detailed spectral analyses using two independent approaches. From the best data set, taken on day 13.8 after outburst, we reconstruct the temperature distribution and derive elemental abundances. We find evidence for at least two distinct temperature components on day 13.8 and a reduction of temperature with time. The X-ray flux decreases as a power law, and the power-law index changes from -5/3 to -8/3 around day 70 after outburst. This can be explained by different decay mechanisms for the hot and cool components. The decay of the hot component and the decrease in temperature are consistent with radiative cooling, while the decay of the cool component can be explained by the expansion of the ejecta. We find overabundances of N and of α elements, which could either represent the composition of the secondary that provides the accreted material or that of the ejecta. The N overabundance indicates CNO-cycled material. From comparisons to abundances for the secondary taken from the literature, we conclude that 20{\%}-40{\%} of the observed nitrogen could originate from the outburst. The overabundance of the α elements is not typical for stars of the spectral type of the secondary in the RSOph system, and white dwarf material might have been mixed into the ejecta. However, no direct measurements of the α elements in the secondary are available, and the continuous accretion may have changed the observable surface composition.",
keywords = "Binaries: symbiotic, Methods: data analysis, Novae, cataclysmic variables, Shock waves, Stars: individual (RSOph), X-rays: stars",
author = "Ness, {J. U.} and Drake, {J. J.} and Sumner Starrfield and Bode, {M. F.} and O'Brien, {T. J.} and A. Evans and Eyres, {S. P S} and Helton, {L. A.} and Osborne, {J. P.} and Page, {K. L.} and C. Schneider and Woodward, {C. E.}",
year = "2009",
doi = "10.1088/0004-6256/137/2/3414",
language = "English (US)",
volume = "137",
pages = "3414--3436",
journal = "Astronomical Journal",
issn = "0004-6256",
publisher = "IOP Publishing Ltd.",
number = "2",

}

TY - JOUR

T1 - High-resolution x-ray spectroscopy of the evolving shock in the 2006 outburst of RS Ophiuchi

AU - Ness, J. U.

AU - Drake, J. J.

AU - Starrfield, Sumner

AU - Bode, M. F.

AU - O'Brien, T. J.

AU - Evans, A.

AU - Eyres, S. P S

AU - Helton, L. A.

AU - Osborne, J. P.

AU - Page, K. L.

AU - Schneider, C.

AU - Woodward, C. E.

PY - 2009

Y1 - 2009

N2 - The evolution of the 2006 outburst of the recurrent nova RSOphiuchi was followed with 12 X-ray grating observations with Chandra and XMM-Newton. We present detailed spectral analyses using two independent approaches. From the best data set, taken on day 13.8 after outburst, we reconstruct the temperature distribution and derive elemental abundances. We find evidence for at least two distinct temperature components on day 13.8 and a reduction of temperature with time. The X-ray flux decreases as a power law, and the power-law index changes from -5/3 to -8/3 around day 70 after outburst. This can be explained by different decay mechanisms for the hot and cool components. The decay of the hot component and the decrease in temperature are consistent with radiative cooling, while the decay of the cool component can be explained by the expansion of the ejecta. We find overabundances of N and of α elements, which could either represent the composition of the secondary that provides the accreted material or that of the ejecta. The N overabundance indicates CNO-cycled material. From comparisons to abundances for the secondary taken from the literature, we conclude that 20%-40% of the observed nitrogen could originate from the outburst. The overabundance of the α elements is not typical for stars of the spectral type of the secondary in the RSOph system, and white dwarf material might have been mixed into the ejecta. However, no direct measurements of the α elements in the secondary are available, and the continuous accretion may have changed the observable surface composition.

AB - The evolution of the 2006 outburst of the recurrent nova RSOphiuchi was followed with 12 X-ray grating observations with Chandra and XMM-Newton. We present detailed spectral analyses using two independent approaches. From the best data set, taken on day 13.8 after outburst, we reconstruct the temperature distribution and derive elemental abundances. We find evidence for at least two distinct temperature components on day 13.8 and a reduction of temperature with time. The X-ray flux decreases as a power law, and the power-law index changes from -5/3 to -8/3 around day 70 after outburst. This can be explained by different decay mechanisms for the hot and cool components. The decay of the hot component and the decrease in temperature are consistent with radiative cooling, while the decay of the cool component can be explained by the expansion of the ejecta. We find overabundances of N and of α elements, which could either represent the composition of the secondary that provides the accreted material or that of the ejecta. The N overabundance indicates CNO-cycled material. From comparisons to abundances for the secondary taken from the literature, we conclude that 20%-40% of the observed nitrogen could originate from the outburst. The overabundance of the α elements is not typical for stars of the spectral type of the secondary in the RSOph system, and white dwarf material might have been mixed into the ejecta. However, no direct measurements of the α elements in the secondary are available, and the continuous accretion may have changed the observable surface composition.

KW - Binaries: symbiotic

KW - Methods: data analysis

KW - Novae, cataclysmic variables

KW - Shock waves

KW - Stars: individual (RSOph)

KW - X-rays: stars

UR - http://www.scopus.com/inward/record.url?scp=66249113147&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=66249113147&partnerID=8YFLogxK

U2 - 10.1088/0004-6256/137/2/3414

DO - 10.1088/0004-6256/137/2/3414

M3 - Article

AN - SCOPUS:66249113147

VL - 137

SP - 3414

EP - 3436

JO - Astronomical Journal

JF - Astronomical Journal

SN - 0004-6256

IS - 2

ER -