Optical spectral monitoring of XTE J1118+480 in outburst: Evidence for a precessing accretion disk

M. A.P. Torres; P. J. Callanan; M. R. Garcia; J. E. McClintock; P. Garnavich; Z. Balog; P. Berlind; W. R. Brown; M. Calkins; A. Mahdavi

doi:10.1086/339282

Optical spectral monitoring of XTE J1118+480 in outburst: Evidence for a precessing accretion disk

M. A.P. Torres
, P. J. Callanan
, M. R. Garcia
, J. E. McClintock
, P. Garnavich
, Z. Balog
, P. Berlind
, W. R. Brown
, M. Calkins
, A. Mahdavi

School of Physics

Research output: Contribution to journal › Article › peer-review

Abstract

We present spectroscopic observations of the X-ray transient XTE J1118+480 acquired during different epochs following the 2000 March outburst. We find that the emission line profiles show variations in their double-peak structure on timescales longer than the 4.1 hr orbital period. We suggest that these changes are due to a tidally driven precessing disk. Doppler imaging of the more intense Balmer lines and the He II λ4686 line shows evidence of a persistent region of enhanced intensity superposed on the disk which is probably associated with the gas stream, the hot spot, or both. We discuss the possible origins of the optical flux in the system and conclude that it may be due to a viscously heated disk.

Original language	English
Pages (from-to)	423-431
Number of pages	9
Journal	Astrophysical Journal
Volume	569
Issue number	1 I
DOIs	https://doi.org/10.1086/339282
Publication status	Published - 10 Apr 2002

Keywords

Accretion, Accretion disks
Binaries: close
X-rays: stars

Access to Document

10.1086/339282

Cite this

@article{24919ea943a34075a3713adb0796bd24,

title = "Optical spectral monitoring of XTE J1118+480 in outburst: Evidence for a precessing accretion disk",

abstract = "We present spectroscopic observations of the X-ray transient XTE J1118+480 acquired during different epochs following the 2000 March outburst. We find that the emission line profiles show variations in their double-peak structure on timescales longer than the 4.1 hr orbital period. We suggest that these changes are due to a tidally driven precessing disk. Doppler imaging of the more intense Balmer lines and the He II λ4686 line shows evidence of a persistent region of enhanced intensity superposed on the disk which is probably associated with the gas stream, the hot spot, or both. We discuss the possible origins of the optical flux in the system and conclude that it may be due to a viscously heated disk.",

keywords = "Accretion, Accretion disks, Binaries: close, X-rays: stars",

author = "Torres, \{M. A.P.\} and Callanan, \{P. J.\} and Garcia, \{M. R.\} and McClintock, \{J. E.\} and P. Garnavich and Z. Balog and P. Berlind and Brown, \{W. R.\} and M. Calkins and A. Mahdavi",

year = "2002",

month = apr,

day = "10",

doi = "10.1086/339282",

language = "English",

volume = "569",

pages = "423--431",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1 I",

}

TY - JOUR

T1 - Optical spectral monitoring of XTE J1118+480 in outburst

T2 - Evidence for a precessing accretion disk

AU - Torres, M. A.P.

AU - Callanan, P. J.

AU - Garcia, M. R.

AU - McClintock, J. E.

AU - Garnavich, P.

AU - Balog, Z.

AU - Berlind, P.

AU - Brown, W. R.

AU - Calkins, M.

AU - Mahdavi, A.

PY - 2002/4/10

Y1 - 2002/4/10

N2 - We present spectroscopic observations of the X-ray transient XTE J1118+480 acquired during different epochs following the 2000 March outburst. We find that the emission line profiles show variations in their double-peak structure on timescales longer than the 4.1 hr orbital period. We suggest that these changes are due to a tidally driven precessing disk. Doppler imaging of the more intense Balmer lines and the He II λ4686 line shows evidence of a persistent region of enhanced intensity superposed on the disk which is probably associated with the gas stream, the hot spot, or both. We discuss the possible origins of the optical flux in the system and conclude that it may be due to a viscously heated disk.

AB - We present spectroscopic observations of the X-ray transient XTE J1118+480 acquired during different epochs following the 2000 March outburst. We find that the emission line profiles show variations in their double-peak structure on timescales longer than the 4.1 hr orbital period. We suggest that these changes are due to a tidally driven precessing disk. Doppler imaging of the more intense Balmer lines and the He II λ4686 line shows evidence of a persistent region of enhanced intensity superposed on the disk which is probably associated with the gas stream, the hot spot, or both. We discuss the possible origins of the optical flux in the system and conclude that it may be due to a viscously heated disk.

KW - Accretion, Accretion disks

KW - Binaries: close

KW - X-rays: stars

UR - https://www.scopus.com/pages/publications/0141539553

U2 - 10.1086/339282

DO - 10.1086/339282

M3 - Article

AN - SCOPUS:0141539553

SN - 0004-637X

VL - 569

SP - 423

EP - 431

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 I

ER -

Optical spectral monitoring of XTE J1118+480 in outburst: Evidence for a precessing accretion disk

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Cite this