Measuring the Expansion and Age of the Nova Shell IPHASX J210204.7+471015

Abstract We present the analysis of XMM-Newton European Photon Imaging Camera (EPIC) observations of the nova shell IPHASX J210204.7+471015. We detect X-ray emission from the progenitor binary star with properties that resemble those of underluminous intermediate polars such as DQ Her: an X-ray-emitting plasma with temperature of TX = (6.4 ± 3.1) × 106 K, a non-thermal X-ray component, and an estimated X-ray luminosity of LX = 1030 erg s−1. Time series analyses unveil the presence of two periods, the dominant with a period of 2.9 ± 0.2 hr, which might be attributed to the spin of the white dwarf, and a secondary of 4.5 ± 0.6 hr that is in line with the orbital period of the binary system derived from optical observations. We do not detect extended X-ray emission as in other nova shells probably due to its relatively old age (130–170 yr) or to its asymmetric disrupted morphology which is suggestive of explosion scenarios different to the symmetric ones assumed in available numerical simulations of nova explosions.

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The First Resolved and Detected Classical Nova Shell in X-Rays: The Shell of Nova Persei 1901

The Astrophysical Journal ◽

10.1086/312069 ◽

1999 ◽

Vol 518 (2) ◽

pp. L111-L114 ◽

Cited By ~ 19

Author(s):

Şölen Balman ◽

Hakki B. Ögelman

Keyword(s):

X Rays ◽

Classical Nova ◽

Nova Shell

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An ancient nova shell around the dwarf nova Z Camelopardalis

Nature ◽

10.1038/nature05576 ◽

2007 ◽

Vol 446 (7132) ◽

pp. 159-162 ◽

Cited By ~ 50

Author(s):

Michael M. Shara ◽

Christopher D. Martin ◽

Mark Seibert ◽

R. Michael Rich ◽

Samir Salim ◽

...

Keyword(s):

Dwarf Nova ◽

Nova Shell

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Extended X-ray emission from the classic nova DQ Her – on the possible presence of a magnetized jet

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1502 ◽

2020 ◽

Vol 495 (4) ◽

pp. 4372-4379

Author(s):

J A Toalá ◽

M A Guerrero ◽

E Santamaría ◽

G Ramos-Larios ◽

L Sabin

Keyword(s):

Major Axis ◽

Bipolar Structure ◽

X Ray ◽

North East ◽

South West ◽

Optical Images ◽

Photon Index ◽

Careful Revision ◽

Nova Shell ◽

Thin Plasma

ABSTRACT We present an analysis of archival Chandra and XMM–Newton observations of the magnetically active cataclysmic variable DQ Her and the shell around it ejected in a nova event in 1934. A careful revision of the Chandra observations confirms previous claims on the presence of extended X-ray emission around DQ Her and reveals that it actually corresponds to a bipolar jet-like structure extending ≃32 arcsec along a direction from north-east to south-west. Therefore, this X-ray emission extends beyond the optical nova shell and is perpendicular to its major axis. The XMM–Newton observations confirm the presence of the extended X-ray emission detected by Chandra, suggesting the additional presence of a diffuse X-ray emission from a hot bubble filling the nova shell. This hot bubble was very likely produced by the explosion that created the nebular shell detected in optical images. The bipolar feature can be modelled by the combination of an optically thin plasma emission component with temperature T ≈ 2 × 106 K and a power-law component with a photon index of Γ = 1.1 ± 0.9. Its X-ray luminosity in the 0.3–5 keV energy range is LX = (2.1 ± 1.3) × 1029 erg s−1, for an electron density ne ≈ 2 cm−3 and a mass mX ≈ 3 × 10−6 M⊙. We suggest that the X-ray bipolar structure in DQ Her is a jet and interpret its non-thermal X-ray emission in terms of a magnetized jet.

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