RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITH INTEGRAL

Publication: Research - peer-reviewJournal article – Annual report year: 2009

Standard

RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITH INTEGRAL. / Fiocchi, M.; Natalucci, L.; Chenevez, Jérôme; Bazzano, A.; Tarana, A.; Ubertini, P.; Brandt, Søren Kristian; Beckmann, V.; Federici, M.; Galis, R.; Hudec, R.

In: Astrophysical Journal, Vol. 693, No. 1, 2009, p. 333-339.

Publication: Research - peer-reviewJournal article – Annual report year: 2009

Harvard

Fiocchi, M, Natalucci, L, Chenevez, J, Bazzano, A, Tarana, A, Ubertini, P, Brandt, SK, Beckmann, V, Federici, M, Galis, R & Hudec, R 2009, 'RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITH INTEGRAL' Astrophysical Journal, vol 693, no. 1, pp. 333-339., 10.1088/0004-637X/693/1/333

APA

Fiocchi, M., Natalucci, L., Chenevez, J., Bazzano, A., Tarana, A., Ubertini, P., Brandt, S. K., Beckmann, V., Federici, M., Galis, R., & Hudec, R. (2009). RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITH INTEGRAL. Astrophysical Journal, 693(1), 333-339. 10.1088/0004-637X/693/1/333

CBE

Fiocchi M, Natalucci L, Chenevez J, Bazzano A, Tarana A, Ubertini P, Brandt SK, Beckmann V, Federici M, Galis R, Hudec R. 2009. RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITH INTEGRAL. Astrophysical Journal. 693(1):333-339. Available from: 10.1088/0004-637X/693/1/333

MLA

Vancouver

Fiocchi M, Natalucci L, Chenevez J, Bazzano A, Tarana A, Ubertini P et al. RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITH INTEGRAL. Astrophysical Journal. 2009;693(1):333-339. Available from: 10.1088/0004-637X/693/1/333

Author

Fiocchi, M.; Natalucci, L.; Chenevez, Jérôme; Bazzano, A.; Tarana, A.; Ubertini, P.; Brandt, Søren Kristian; Beckmann, V.; Federici, M.; Galis, R.; Hudec, R. / RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITH INTEGRAL.

In: Astrophysical Journal, Vol. 693, No. 1, 2009, p. 333-339.

Publication: Research - peer-reviewJournal article – Annual report year: 2009

Bibtex

@article{54fe39b80ae84b3c9ee1897cb654cda2,
title = "RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITH INTEGRAL",
publisher = "Institute of Physics Publishing, Inc",
author = "M. Fiocchi and L. Natalucci and Jérôme Chenevez and A. Bazzano and A. Tarana and P. Ubertini and Brandt, {Søren Kristian} and V. Beckmann and M. Federici and R. Galis and R. Hudec",
year = "2009",
doi = "10.1088/0004-637X/693/1/333",
volume = "693",
number = "1",
pages = "333--339",
journal = "Astrophysical Journal",
issn = "0004-637X",

}

RIS

TY - JOUR

T1 - RENEWED ACTIVITY FROM THE X-RAY TRANSIENT SAXJ 1810.8-2609 WITH INTEGRAL

A1 - Fiocchi,M.

A1 - Natalucci,L.

A1 - Chenevez,Jérôme

A1 - Bazzano,A.

A1 - Tarana,A.

A1 - Ubertini,P.

A1 - Brandt,Søren Kristian

A1 - Beckmann,V.

A1 - Federici,M.

A1 - Galis,R.

A1 - Hudec,R.

AU - Fiocchi,M.

AU - Natalucci,L.

AU - Chenevez,Jérôme

AU - Bazzano,A.

AU - Tarana,A.

AU - Ubertini,P.

AU - Brandt,Søren Kristian

AU - Beckmann,V.

AU - Federici,M.

AU - Galis,R.

AU - Hudec,R.

PB - Institute of Physics Publishing, Inc

PY - 2009

Y1 - 2009

N2 - We report on the results of International Gamma-Ray Astrophysics Laboratory (INTEGRAL) observations of the neutron star low-mass X-ray binary SAX J1810.8-2609 during its latest active phase in 2007 August. The current outburst is the first one since 1998 and the derived luminosity is 1.1-2.6 x 10(36) erg s(-1) in the 20-100 keV energy range. This low outburst luminosity and the long-term time-average accretion rate of similar to 5 x 10(-12) M-circle dot yr(-1) suggest that SAX J1810.8-2609 is a faint soft X-ray transient. During the flux increase, spectra are consistent with a thermal Comptonization model with a temperature plasma of kT(e) similar to 23-30 keV and an optical depth of tau similar to 1.2-1.5, independent of the luminosity of the system. This is a typical low hard spectral state for which the X-ray emission is attributed to the upscattering of soft seed photons by a hot, optically thin electron plasma. During the decay, spectra have a different shape, the high energy tail being compatible with a single power law. This confirm similar behavior observed by BeppoSAX during the previous outburst, with the absence of visible cutoff in the hard X-ray spectrum. INTEGRAL/JEM-X instrument observed four X-ray bursts in Fall 2007. The first one has the highest peak flux (approximate to 3.5 crab in 3-25 keV) giving an upper limit to the distance of the source of about 5.7 kpc, for a L-Edd approximate to 3.8 x 10(38) erg s(-1). The observed recurrence time of similar to 1.2 days and the ratio of the total energy emitted in the persistent flux to that emitted in the bursts (alpha similar to 73) allow us to conclude that the burst fuel was composed by mixed hydrogen and helium with X >= 0.4.

AB - We report on the results of International Gamma-Ray Astrophysics Laboratory (INTEGRAL) observations of the neutron star low-mass X-ray binary SAX J1810.8-2609 during its latest active phase in 2007 August. The current outburst is the first one since 1998 and the derived luminosity is 1.1-2.6 x 10(36) erg s(-1) in the 20-100 keV energy range. This low outburst luminosity and the long-term time-average accretion rate of similar to 5 x 10(-12) M-circle dot yr(-1) suggest that SAX J1810.8-2609 is a faint soft X-ray transient. During the flux increase, spectra are consistent with a thermal Comptonization model with a temperature plasma of kT(e) similar to 23-30 keV and an optical depth of tau similar to 1.2-1.5, independent of the luminosity of the system. This is a typical low hard spectral state for which the X-ray emission is attributed to the upscattering of soft seed photons by a hot, optically thin electron plasma. During the decay, spectra have a different shape, the high energy tail being compatible with a single power law. This confirm similar behavior observed by BeppoSAX during the previous outburst, with the absence of visible cutoff in the hard X-ray spectrum. INTEGRAL/JEM-X instrument observed four X-ray bursts in Fall 2007. The first one has the highest peak flux (approximate to 3.5 crab in 3-25 keV) giving an upper limit to the distance of the source of about 5.7 kpc, for a L-Edd approximate to 3.8 x 10(38) erg s(-1). The observed recurrence time of similar to 1.2 days and the ratio of the total energy emitted in the persistent flux to that emitted in the bursts (alpha similar to 73) allow us to conclude that the burst fuel was composed by mixed hydrogen and helium with X >= 0.4.

KW - radiation mechanisms: non-thermal

KW - stars: neutron

KW - stars: individual (SAX J1810.8-2609)

KW - gamma rays: observations

KW - X-rays: binaries

UR - http://www.iop.org/EJ/abstract/0004-637X/693/1/333/

U2 - 10.1088/0004-637X/693/1/333

DO - 10.1088/0004-637X/693/1/333

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

VL - 693

SP - 333

EP - 339

ER -