The SSS phase of RS ophiuchi observed with Chandra and XMM-Newton. I. Data and preliminary modeling

J. U. Ness; Sumner Starrfield; A. P. Beardmore; M. F. Bode; J. J. Drake; A. Evans; R. D. Gehrz; M. R. Goad; R. Gonzalez-Riestra; P. Hauschildt; J. Krautter; T. J. O'Brien; J. P. Osborne; K. L. Page; R. A. Schönrich; C. E. Woodward

doi:10.1086/519676

The SSS phase of RS ophiuchi observed with Chandra and XMM-Newton. I. Data and preliminary modeling

J. U. Ness, Sumner Starrfield, A. P. Beardmore, M. F. Bode, J. J. Drake, A. Evans, R. D. Gehrz, M. R. Goad, R. Gonzalez-Riestra, P. Hauschildt, J. Krautter, T. J. O'Brien, J. P. Osborne, K. L. Page, R. A. Schönrich, C. E. Woodward

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Abstract

The phase of supersoft source (SSS) emission of the sixth recorded outburst of the recurrent nova RS Oph was observed on days 39.7 and 66.9 after outburst with Chandra and on day 54.0 with XMM-Newton. A ∼35 s period on day 54.0 originates from the SSS emission and not from the shock. We discuss the bound-free absorption by neutral elements in the line of sight, resonance absorption lines plus self-absorbed emission-line components, collisionally excited emission lines from the shock, He-like intersystem lines, and spectral changes during an episode of highamplitude variability. We find a decrease of the oxygen K-shell absorption edge that can be explained by photoionization of oxygen. The absorption component has average velocities of -1286 ± 267 km s^-1 on day 39.7 and of -771 ± 65 km s^-1 on day 66.9. The wavelengths of the emission-line components are at rest wavelengths, as confirmed by measurements of non-self-absorbed He-like intersystem lines. We found collisionally excited emission lines from the radiatively cooling shock at wavelengths shorter than 15 Å that are systematically blueshifted by -526 ± 114 km s^-1 on day 39.7 and are fading. We found anomalous He-likef/i ratios, which indicates either high densities or significant UV radiation near the plasma where the emission lines are formed. During the phase of strong variability the spectral hardness light curve overlies the total light curve when shifted by 1000 s. This can be explained by photoionization of neutral oxygen in the line of sight if the densities are of order 10 ¹⁰-10¹¹ cm^-3.

Original language	English (US)
Pages (from-to)	1334-1348
Number of pages	15
Journal	Astrophysical Journal
Volume	665
Issue number	2 I
DOIs	https://doi.org/10.1086/519676
State	Published - Aug 10 2007

Keywords

Cataclysmic variables
Novae
Stars: Individual (RS Ophiuchi)
X-rays: Stars

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/519676

Cite this

Ness, J. U., Starrfield, S., Beardmore, A. P., Bode, M. F., Drake, J. J., Evans, A., Gehrz, R. D., Goad, M. R., Gonzalez-Riestra, R., Hauschildt, P., Krautter, J., O'Brien, T. J., Osborne, J. P., Page, K. L., Schönrich, R. A., & Woodward, C. E. (2007). The SSS phase of RS ophiuchi observed with Chandra and XMM-Newton. I. Data and preliminary modeling. Astrophysical Journal, 665(2 I), 1334-1348. https://doi.org/10.1086/519676

Ness, JU, Starrfield, S, Beardmore, AP, Bode, MF, Drake, JJ, Evans, A, Gehrz, RD, Goad, MR, Gonzalez-Riestra, R, Hauschildt, P, Krautter, J, O'Brien, TJ, Osborne, JP, Page, KL, Schönrich, RA & Woodward, CE 2007, 'The SSS phase of RS ophiuchi observed with Chandra and XMM-Newton. I. Data and preliminary modeling', Astrophysical Journal, vol. 665, no. 2 I, pp. 1334-1348. https://doi.org/10.1086/519676

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title = "The SSS phase of RS ophiuchi observed with Chandra and XMM-Newton. I. Data and preliminary modeling",

abstract = "The phase of supersoft source (SSS) emission of the sixth recorded outburst of the recurrent nova RS Oph was observed on days 39.7 and 66.9 after outburst with Chandra and on day 54.0 with XMM-Newton. A ∼35 s period on day 54.0 originates from the SSS emission and not from the shock. We discuss the bound-free absorption by neutral elements in the line of sight, resonance absorption lines plus self-absorbed emission-line components, collisionally excited emission lines from the shock, He-like intersystem lines, and spectral changes during an episode of highamplitude variability. We find a decrease of the oxygen K-shell absorption edge that can be explained by photoionization of oxygen. The absorption component has average velocities of -1286 ± 267 km s-1 on day 39.7 and of -771 ± 65 km s-1 on day 66.9. The wavelengths of the emission-line components are at rest wavelengths, as confirmed by measurements of non-self-absorbed He-like intersystem lines. We found collisionally excited emission lines from the radiatively cooling shock at wavelengths shorter than 15 {\AA} that are systematically blueshifted by -526 ± 114 km s-1 on day 39.7 and are fading. We found anomalous He-likef/i ratios, which indicates either high densities or significant UV radiation near the plasma where the emission lines are formed. During the phase of strong variability the spectral hardness light curve overlies the total light curve when shifted by 1000 s. This can be explained by photoionization of neutral oxygen in the line of sight if the densities are of order 10 10-1011 cm-3.",

keywords = "Cataclysmic variables, Novae, Stars: Individual (RS Ophiuchi), X-rays: Stars",

author = "Ness, {J. U.} and Sumner Starrfield and Beardmore, {A. P.} and Bode, {M. F.} and Drake, {J. J.} and A. Evans and Gehrz, {R. D.} and Goad, {M. R.} and R. Gonzalez-Riestra and P. Hauschildt and J. Krautter and O'Brien, {T. J.} and Osborne, {J. P.} and Page, {K. L.} and Sch{\"o}nrich, {R. A.} and Woodward, {C. E.}",

year = "2007",

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doi = "10.1086/519676",

language = "English (US)",

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T1 - The SSS phase of RS ophiuchi observed with Chandra and XMM-Newton. I. Data and preliminary modeling

AU - Ness, J. U.

AU - Starrfield, Sumner

AU - Beardmore, A. P.

AU - Bode, M. F.

AU - Drake, J. J.

AU - Evans, A.

AU - Gehrz, R. D.

AU - Goad, M. R.

AU - Gonzalez-Riestra, R.

AU - Hauschildt, P.

AU - Krautter, J.

AU - O'Brien, T. J.

AU - Osborne, J. P.

AU - Page, K. L.

AU - Schönrich, R. A.

AU - Woodward, C. E.

PY - 2007/8/10

Y1 - 2007/8/10

N2 - The phase of supersoft source (SSS) emission of the sixth recorded outburst of the recurrent nova RS Oph was observed on days 39.7 and 66.9 after outburst with Chandra and on day 54.0 with XMM-Newton. A ∼35 s period on day 54.0 originates from the SSS emission and not from the shock. We discuss the bound-free absorption by neutral elements in the line of sight, resonance absorption lines plus self-absorbed emission-line components, collisionally excited emission lines from the shock, He-like intersystem lines, and spectral changes during an episode of highamplitude variability. We find a decrease of the oxygen K-shell absorption edge that can be explained by photoionization of oxygen. The absorption component has average velocities of -1286 ± 267 km s-1 on day 39.7 and of -771 ± 65 km s-1 on day 66.9. The wavelengths of the emission-line components are at rest wavelengths, as confirmed by measurements of non-self-absorbed He-like intersystem lines. We found collisionally excited emission lines from the radiatively cooling shock at wavelengths shorter than 15 Å that are systematically blueshifted by -526 ± 114 km s-1 on day 39.7 and are fading. We found anomalous He-likef/i ratios, which indicates either high densities or significant UV radiation near the plasma where the emission lines are formed. During the phase of strong variability the spectral hardness light curve overlies the total light curve when shifted by 1000 s. This can be explained by photoionization of neutral oxygen in the line of sight if the densities are of order 10 10-1011 cm-3.

AB - The phase of supersoft source (SSS) emission of the sixth recorded outburst of the recurrent nova RS Oph was observed on days 39.7 and 66.9 after outburst with Chandra and on day 54.0 with XMM-Newton. A ∼35 s period on day 54.0 originates from the SSS emission and not from the shock. We discuss the bound-free absorption by neutral elements in the line of sight, resonance absorption lines plus self-absorbed emission-line components, collisionally excited emission lines from the shock, He-like intersystem lines, and spectral changes during an episode of highamplitude variability. We find a decrease of the oxygen K-shell absorption edge that can be explained by photoionization of oxygen. The absorption component has average velocities of -1286 ± 267 km s-1 on day 39.7 and of -771 ± 65 km s-1 on day 66.9. The wavelengths of the emission-line components are at rest wavelengths, as confirmed by measurements of non-self-absorbed He-like intersystem lines. We found collisionally excited emission lines from the radiatively cooling shock at wavelengths shorter than 15 Å that are systematically blueshifted by -526 ± 114 km s-1 on day 39.7 and are fading. We found anomalous He-likef/i ratios, which indicates either high densities or significant UV radiation near the plasma where the emission lines are formed. During the phase of strong variability the spectral hardness light curve overlies the total light curve when shifted by 1000 s. This can be explained by photoionization of neutral oxygen in the line of sight if the densities are of order 10 10-1011 cm-3.

KW - Cataclysmic variables

KW - Novae

KW - Stars: Individual (RS Ophiuchi)

KW - X-rays: Stars

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U2 - 10.1086/519676

DO - 10.1086/519676

M3 - Article

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SN - 0004-637X

VL - 665

SP - 1334

EP - 1348

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2 I

ER -

The SSS phase of RS ophiuchi observed with Chandra and XMM-Newton. I. Data and preliminary modeling

Abstract

Keywords

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