Collimation and asymmetry of the hot blast wave from the recurrent nova V745 Sco

Jeremy J. Drake, Laura Delgado, J. Martin Laming, Sumner Starrfield, Vinay Kashyap, Salvatore Orlando, Kim L. Page, M. Hernanz, J. U. Ness, R. D. Gehrz, Daan Van Rossum, Charles E. Woodward

Research output: Contribution to journalArticle

4 Citations (Scopus)

Abstract

The recurrent symbiotic nova V745 Sco exploded on 2014 February 6 and was observed on February 22 and 23 by the Chandra X-ray Observatory Transmission Grating Spectrometers. By that time the supersoft source phase had already ended, and Chandra spectra are consistent with emission from a hot, shock-heated circumstellar medium with temperatures exceeding 107 K. X-ray line profiles are more sharply peaked than expected for a spherically symmetric blast wave, with a full width at zero intensity of approximately 2400 km s-1, an FWHM of 1200 ± 30 km s-1, and an average net blueshift of 165 ± 10 km s-1. The red wings of lines are increasingly absorbed toward longer wavelengths by material within the remnant. We conclude that the blast wave was sculpted by an aspherical circumstellar medium in which an equatorial density enhancement plays a role, as in earlier symbiotic nova explosions. Expansion of the dominant X-ray-emitting material is aligned close to the plane of the sky and is most consistent with an orbit seen close to face-on. Comparison of an analytical blast wave model with the X-ray spectra, Swift observations, and near-infrared line widths indicates that the explosion energy was approximately 1043 erg and confirms an ejected mass of approximately 10-7 M Ȯ. The total mass lost is an order of magnitude lower than the accreted mass required to have initiated the explosion, indicating that the white dwarf is gaining mass and is a Type Ia supernova progenitor candidate.

Original languageEnglish (US)
Article number95
JournalAstrophysical Journal
Volume825
Issue number2
DOIs
StatePublished - Jul 10 2016

Fingerprint

collimation
blasts
asymmetry
explosions
explosion
x rays
wings
erg
supernovae
sky
near infrared
observatories
spectrometer
observatory
shock
gratings
spectrometers
wavelength
orbits
expansion

Keywords

  • novae, cataclysmic variables
  • shock waves
  • stars: individual (V745 Sco)
  • X-rays: binaries
  • X-rays: stars

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Drake, J. J., Delgado, L., Laming, J. M., Starrfield, S., Kashyap, V., Orlando, S., ... Woodward, C. E. (2016). Collimation and asymmetry of the hot blast wave from the recurrent nova V745 Sco. Astrophysical Journal, 825(2), [95]. https://doi.org/10.3847/0004-637X/825/2/95

Collimation and asymmetry of the hot blast wave from the recurrent nova V745 Sco. / Drake, Jeremy J.; Delgado, Laura; Laming, J. Martin; Starrfield, Sumner; Kashyap, Vinay; Orlando, Salvatore; Page, Kim L.; Hernanz, M.; Ness, J. U.; Gehrz, R. D.; Van Rossum, Daan; Woodward, Charles E.

In: Astrophysical Journal, Vol. 825, No. 2, 95, 10.07.2016.

Research output: Contribution to journalArticle

Drake, JJ, Delgado, L, Laming, JM, Starrfield, S, Kashyap, V, Orlando, S, Page, KL, Hernanz, M, Ness, JU, Gehrz, RD, Van Rossum, D & Woodward, CE 2016, 'Collimation and asymmetry of the hot blast wave from the recurrent nova V745 Sco', Astrophysical Journal, vol. 825, no. 2, 95. https://doi.org/10.3847/0004-637X/825/2/95
Drake, Jeremy J. ; Delgado, Laura ; Laming, J. Martin ; Starrfield, Sumner ; Kashyap, Vinay ; Orlando, Salvatore ; Page, Kim L. ; Hernanz, M. ; Ness, J. U. ; Gehrz, R. D. ; Van Rossum, Daan ; Woodward, Charles E. / Collimation and asymmetry of the hot blast wave from the recurrent nova V745 Sco. In: Astrophysical Journal. 2016 ; Vol. 825, No. 2.
@article{e4f6effe9f7b4d939a587fe03b5d7440,
title = "Collimation and asymmetry of the hot blast wave from the recurrent nova V745 Sco",
abstract = "The recurrent symbiotic nova V745 Sco exploded on 2014 February 6 and was observed on February 22 and 23 by the Chandra X-ray Observatory Transmission Grating Spectrometers. By that time the supersoft source phase had already ended, and Chandra spectra are consistent with emission from a hot, shock-heated circumstellar medium with temperatures exceeding 107 K. X-ray line profiles are more sharply peaked than expected for a spherically symmetric blast wave, with a full width at zero intensity of approximately 2400 km s-1, an FWHM of 1200 ± 30 km s-1, and an average net blueshift of 165 ± 10 km s-1. The red wings of lines are increasingly absorbed toward longer wavelengths by material within the remnant. We conclude that the blast wave was sculpted by an aspherical circumstellar medium in which an equatorial density enhancement plays a role, as in earlier symbiotic nova explosions. Expansion of the dominant X-ray-emitting material is aligned close to the plane of the sky and is most consistent with an orbit seen close to face-on. Comparison of an analytical blast wave model with the X-ray spectra, Swift observations, and near-infrared line widths indicates that the explosion energy was approximately 1043 erg and confirms an ejected mass of approximately 10-7 M Ȯ. The total mass lost is an order of magnitude lower than the accreted mass required to have initiated the explosion, indicating that the white dwarf is gaining mass and is a Type Ia supernova progenitor candidate.",
keywords = "novae, cataclysmic variables, shock waves, stars: individual (V745 Sco), X-rays: binaries, X-rays: stars",
author = "Drake, {Jeremy J.} and Laura Delgado and Laming, {J. Martin} and Sumner Starrfield and Vinay Kashyap and Salvatore Orlando and Page, {Kim L.} and M. Hernanz and Ness, {J. U.} and Gehrz, {R. D.} and {Van Rossum}, Daan and Woodward, {Charles E.}",
year = "2016",
month = "7",
day = "10",
doi = "10.3847/0004-637X/825/2/95",
language = "English (US)",
volume = "825",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

TY - JOUR

T1 - Collimation and asymmetry of the hot blast wave from the recurrent nova V745 Sco

AU - Drake, Jeremy J.

AU - Delgado, Laura

AU - Laming, J. Martin

AU - Starrfield, Sumner

AU - Kashyap, Vinay

AU - Orlando, Salvatore

AU - Page, Kim L.

AU - Hernanz, M.

AU - Ness, J. U.

AU - Gehrz, R. D.

AU - Van Rossum, Daan

AU - Woodward, Charles E.

PY - 2016/7/10

Y1 - 2016/7/10

N2 - The recurrent symbiotic nova V745 Sco exploded on 2014 February 6 and was observed on February 22 and 23 by the Chandra X-ray Observatory Transmission Grating Spectrometers. By that time the supersoft source phase had already ended, and Chandra spectra are consistent with emission from a hot, shock-heated circumstellar medium with temperatures exceeding 107 K. X-ray line profiles are more sharply peaked than expected for a spherically symmetric blast wave, with a full width at zero intensity of approximately 2400 km s-1, an FWHM of 1200 ± 30 km s-1, and an average net blueshift of 165 ± 10 km s-1. The red wings of lines are increasingly absorbed toward longer wavelengths by material within the remnant. We conclude that the blast wave was sculpted by an aspherical circumstellar medium in which an equatorial density enhancement plays a role, as in earlier symbiotic nova explosions. Expansion of the dominant X-ray-emitting material is aligned close to the plane of the sky and is most consistent with an orbit seen close to face-on. Comparison of an analytical blast wave model with the X-ray spectra, Swift observations, and near-infrared line widths indicates that the explosion energy was approximately 1043 erg and confirms an ejected mass of approximately 10-7 M Ȯ. The total mass lost is an order of magnitude lower than the accreted mass required to have initiated the explosion, indicating that the white dwarf is gaining mass and is a Type Ia supernova progenitor candidate.

AB - The recurrent symbiotic nova V745 Sco exploded on 2014 February 6 and was observed on February 22 and 23 by the Chandra X-ray Observatory Transmission Grating Spectrometers. By that time the supersoft source phase had already ended, and Chandra spectra are consistent with emission from a hot, shock-heated circumstellar medium with temperatures exceeding 107 K. X-ray line profiles are more sharply peaked than expected for a spherically symmetric blast wave, with a full width at zero intensity of approximately 2400 km s-1, an FWHM of 1200 ± 30 km s-1, and an average net blueshift of 165 ± 10 km s-1. The red wings of lines are increasingly absorbed toward longer wavelengths by material within the remnant. We conclude that the blast wave was sculpted by an aspherical circumstellar medium in which an equatorial density enhancement plays a role, as in earlier symbiotic nova explosions. Expansion of the dominant X-ray-emitting material is aligned close to the plane of the sky and is most consistent with an orbit seen close to face-on. Comparison of an analytical blast wave model with the X-ray spectra, Swift observations, and near-infrared line widths indicates that the explosion energy was approximately 1043 erg and confirms an ejected mass of approximately 10-7 M Ȯ. The total mass lost is an order of magnitude lower than the accreted mass required to have initiated the explosion, indicating that the white dwarf is gaining mass and is a Type Ia supernova progenitor candidate.

KW - novae, cataclysmic variables

KW - shock waves

KW - stars: individual (V745 Sco)

KW - X-rays: binaries

KW - X-rays: stars

UR - http://www.scopus.com/inward/record.url?scp=84978513158&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84978513158&partnerID=8YFLogxK

U2 - 10.3847/0004-637X/825/2/95

DO - 10.3847/0004-637X/825/2/95

M3 - Article

VL - 825

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 95

ER -