X-ray spectrum of the Rapid Burster using the Chandra HETGS

H. L. Marshall; R. Rutledge; D. W. Fox; J. M. Miller; R. Guerriero; E. Morgan; M. Van Der Klis; L. Bildsten; T. Dotani; W. H.G. Lewin

doi:10.1086/321142

X-ray spectrum of the Rapid Burster using the Chandra HETGS

H. L. Marshall, R. Rutledge, D. W. Fox, J. M. Miller, R. Guerriero, E. Morgan, M. Van Der Klis, L. Bildsten, T. Dotani, W. H.G. Lewin

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15 Scopus citations

Abstract

We present observations of the Rapid Burster (RB, also known as MXB 1730-335) using the Chandra High Energy Transmission Grating Spectrometer. The average interval between type II (accretion) bursts was about 40 s. There was one type I (thermonuclear flash) burst and about 20 minibursts that are probably type II bursts whose peak flux is 10%-40% of the average peak flux of the other type II bursts. The time-averaged spectra of the type II bursts are well fitted by a blackbody with a temperature of kT = 1.6 keV, a radius of 8.9 km for a distance of 8.6 kpc, and an interstellar column density of 1.7 × 10²² cm^-2. No narrow emission or absorption lines were clearly detected. The 3 σ upper limits to the equivalent widths of any features are less than 10 eV in the 1.1-7.0 keV band and as small as 1.5 eV near 1.7 keV. We suggest that Comptonization destroys absorption features such as the resonance line of Fe XXVI.

Original language	English (US)
Pages (from-to)	21-25
Number of pages	5
Journal	Astronomical Journal
Volume	122
Issue number	1
DOIs	https://doi.org/10.1086/321142
State	Published - Jul 2001

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/321142

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@article{e112d79d88994567bd45fc09091f085d,

title = "X-ray spectrum of the Rapid Burster using the Chandra HETGS",

abstract = "We present observations of the Rapid Burster (RB, also known as MXB 1730-335) using the Chandra High Energy Transmission Grating Spectrometer. The average interval between type II (accretion) bursts was about 40 s. There was one type I (thermonuclear flash) burst and about 20 minibursts that are probably type II bursts whose peak flux is 10%-40% of the average peak flux of the other type II bursts. The time-averaged spectra of the type II bursts are well fitted by a blackbody with a temperature of kT = 1.6 keV, a radius of 8.9 km for a distance of 8.6 kpc, and an interstellar column density of 1.7 × 1022 cm-2. No narrow emission or absorption lines were clearly detected. The 3 σ upper limits to the equivalent widths of any features are less than 10 eV in the 1.1-7.0 keV band and as small as 1.5 eV near 1.7 keV. We suggest that Comptonization destroys absorption features such as the resonance line of Fe XXVI.",

author = "Marshall, {H. L.} and R. Rutledge and Fox, {D. W.} and Miller, {J. M.} and R. Guerriero and E. Morgan and {Van Der Klis}, M. and L. Bildsten and T. Dotani and Lewin, {W. H.G.}",

year = "2001",

month = jul,

doi = "10.1086/321142",

language = "English (US)",

volume = "122",

pages = "21--25",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "IOP Publishing Ltd.",

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TY - JOUR

T1 - X-ray spectrum of the Rapid Burster using the Chandra HETGS

AU - Marshall, H. L.

AU - Rutledge, R.

AU - Fox, D. W.

AU - Miller, J. M.

AU - Guerriero, R.

AU - Morgan, E.

AU - Van Der Klis, M.

AU - Bildsten, L.

AU - Dotani, T.

AU - Lewin, W. H.G.

PY - 2001/7

Y1 - 2001/7

N2 - We present observations of the Rapid Burster (RB, also known as MXB 1730-335) using the Chandra High Energy Transmission Grating Spectrometer. The average interval between type II (accretion) bursts was about 40 s. There was one type I (thermonuclear flash) burst and about 20 minibursts that are probably type II bursts whose peak flux is 10%-40% of the average peak flux of the other type II bursts. The time-averaged spectra of the type II bursts are well fitted by a blackbody with a temperature of kT = 1.6 keV, a radius of 8.9 km for a distance of 8.6 kpc, and an interstellar column density of 1.7 × 1022 cm-2. No narrow emission or absorption lines were clearly detected. The 3 σ upper limits to the equivalent widths of any features are less than 10 eV in the 1.1-7.0 keV band and as small as 1.5 eV near 1.7 keV. We suggest that Comptonization destroys absorption features such as the resonance line of Fe XXVI.

AB - We present observations of the Rapid Burster (RB, also known as MXB 1730-335) using the Chandra High Energy Transmission Grating Spectrometer. The average interval between type II (accretion) bursts was about 40 s. There was one type I (thermonuclear flash) burst and about 20 minibursts that are probably type II bursts whose peak flux is 10%-40% of the average peak flux of the other type II bursts. The time-averaged spectra of the type II bursts are well fitted by a blackbody with a temperature of kT = 1.6 keV, a radius of 8.9 km for a distance of 8.6 kpc, and an interstellar column density of 1.7 × 1022 cm-2. No narrow emission or absorption lines were clearly detected. The 3 σ upper limits to the equivalent widths of any features are less than 10 eV in the 1.1-7.0 keV band and as small as 1.5 eV near 1.7 keV. We suggest that Comptonization destroys absorption features such as the resonance line of Fe XXVI.

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U2 - 10.1086/321142

DO - 10.1086/321142

M3 - Article

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SN - 0004-6256

VL - 122

SP - 21

EP - 25

JO - Astronomical Journal

JF - Astronomical Journal

IS - 1

ER -

X-ray spectrum of the Rapid Burster using the Chandra HETGS

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