Chandra observation of the Big Dipper X 1624-490

Rosario Iaria; Tiziana Di Salvo; Antonino D'Ai'; Natale Robba; Giuseppe Lavagetto

Chandra observation of the Big Dipper X 1624-490

Rosario Iaria, Tiziana Di Salvo, Antonino D'Ai', Natale Robba, Giuseppe Lavagetto

Fisica e Chimica - Emilio Segrè

Risultato della ricerca: Article › peer review

13 Citazioni (Scopus)

Abstract

We present the results of a 73 ks long Chandra observation of the dipping source X 1624 - 490. During the observation a complex dip lasting 4 h is observed. We analyse the persistent emission detecting, for the first time in the 1st-order spectra of X 1624 - 490, an absorption line associated to Ca XX We confirm the presence of the Fe XXV K-alpha and Fe XXVI K-alpha absorption lines with a larger accuracy with respect to a previous XMM observation. Assuming that the line widths are due to a bulk motion or a turbulence associated to the coronal activity, we estimate that the lines have been produced in a photoionized absorber between the coronal radius and the outer edge of the accretion disk.

Lingua originale	English
pagine (da-a)	289-295
Numero di pagine	7
Rivista	ASTRONOMY & ASTROPHYSICS
Volume	463
Stato di pubblicazione	Published - 2007

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Fingerprint Entra nei temi di ricerca di 'Chandra observation of the Big Dipper X 1624-490'. Insieme formano una fingerprint unica.

Cita questo

@article{0ecb2743d93247a4b81491d4e73bd292,

title = "Chandra observation of the Big Dipper X 1624-490",

abstract = "We present the results of a 73 ks long Chandra observation of the dipping source X 1624 - 490. During the observation a complex dip lasting 4 h is observed. We analyse the persistent emission detecting, for the first time in the 1st-order spectra of X 1624 - 490, an absorption line associated to Ca XX We confirm the presence of the Fe XXV K-alpha and Fe XXVI K-alpha absorption lines with a larger accuracy with respect to a previous XMM observation. Assuming that the line widths are due to a bulk motion or a turbulence associated to the coronal activity, we estimate that the lines have been produced in a photoionized absorber between the coronal radius and the outer edge of the accretion disk.",

keywords = "accretion, accretion disks; stars : individual : X 1624-490; stars : neutron; X-rays : stars; X-rays : binaries; X-rays : general, accretion, accretion disks; stars : individual : X 1624-490; stars : neutron; X-rays : stars; X-rays : binaries; X-rays : general",

author = "Rosario Iaria and {Di Salvo}, Tiziana and Antonino D'Ai' and Natale Robba and Giuseppe Lavagetto",

year = "2007",

language = "English",

volume = "463",

pages = "289--295",

journal = "ASTRONOMY & ASTROPHYSICS",

issn = "0004-6361",

}

TY - JOUR

T1 - Chandra observation of the Big Dipper X 1624-490

AU - Iaria, Rosario

AU - Di Salvo, Tiziana

AU - D'Ai', Antonino

AU - Robba, Natale

AU - Lavagetto, Giuseppe

PY - 2007

Y1 - 2007

N2 - We present the results of a 73 ks long Chandra observation of the dipping source X 1624 - 490. During the observation a complex dip lasting 4 h is observed. We analyse the persistent emission detecting, for the first time in the 1st-order spectra of X 1624 - 490, an absorption line associated to Ca XX We confirm the presence of the Fe XXV K-alpha and Fe XXVI K-alpha absorption lines with a larger accuracy with respect to a previous XMM observation. Assuming that the line widths are due to a bulk motion or a turbulence associated to the coronal activity, we estimate that the lines have been produced in a photoionized absorber between the coronal radius and the outer edge of the accretion disk.

AB - We present the results of a 73 ks long Chandra observation of the dipping source X 1624 - 490. During the observation a complex dip lasting 4 h is observed. We analyse the persistent emission detecting, for the first time in the 1st-order spectra of X 1624 - 490, an absorption line associated to Ca XX We confirm the presence of the Fe XXV K-alpha and Fe XXVI K-alpha absorption lines with a larger accuracy with respect to a previous XMM observation. Assuming that the line widths are due to a bulk motion or a turbulence associated to the coronal activity, we estimate that the lines have been produced in a photoionized absorber between the coronal radius and the outer edge of the accretion disk.

KW - accretion

KW - accretion disks; stars : individual : X 1624-490; stars : neutron; X-rays : stars; X-rays : binaries; X-rays : general

KW - accretion

KW - accretion disks; stars : individual : X 1624-490; stars : neutron; X-rays : stars; X-rays : binaries; X-rays : general

UR - http://hdl.handle.net/10447/27006

M3 - Article

VL - 463

SP - 289

EP - 295

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

ER -