Chandra observation of the Big Dipper X 1624–490
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 $\ion{C...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2007-02, Vol.463 (1), p.289-295 |
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| container_title | Astronomy and astrophysics (Berlin) |
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| creator | Iaria, R. Lavagetto, G. D'Aí, A. Di Salvo, T. Robba, N. R. |
| description | 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 $\ion{Ca}{xx}$. We confirm the presence of the $\ion{Fe}{xxv}$ Kα and $\ion{Fe}{xxvi}$ Kα 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. |
| doi_str_mv | 10.1051/0004-6361:20065862 |
| format | Article |
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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.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361:20065862</identifier><identifier>CODEN: AAEJAF</identifier><language>eng</language><publisher>Les Ulis: EDP Sciences</publisher><subject>accretion ; accretion disks ; Astronomy ; Earth, ocean, space ; Exact sciences and technology ; stars: individual: X 1624–490 ; stars: neutron ; X-rays: binaries ; X-rays: general ; X-rays: stars</subject><ispartof>Astronomy and astrophysics (Berlin), 2007-02, Vol.463 (1), p.289-295</ispartof><rights>2007 INIST-CNRS</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c390t-d64e25e26fc17758a994d75d65cf7b7b51ad0210f917ae896a3a6981aea76a853</citedby><cites>FETCH-LOGICAL-c390t-d64e25e26fc17758a994d75d65cf7b7b51ad0210f917ae896a3a6981aea76a853</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,3714,27901,27902</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=18485153$$DView record in Pascal Francis$$Hfree_for_read</backlink></links><search><creatorcontrib>Iaria, R.</creatorcontrib><creatorcontrib>Lavagetto, G.</creatorcontrib><creatorcontrib>D'Aí, A.</creatorcontrib><creatorcontrib>Di Salvo, T.</creatorcontrib><creatorcontrib>Robba, N. 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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.</description><subject>accretion</subject><subject>accretion disks</subject><subject>Astronomy</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>stars: individual: X 1624–490</subject><subject>stars: neutron</subject><subject>X-rays: binaries</subject><subject>X-rays: general</subject><subject>X-rays: stars</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2007</creationdate><recordtype>article</recordtype><recordid>eNpFkM1OwkAUhSdGExF9AVfd6K46_z_uBERNMMaogbiZXNqpVEtbZ4rRne_gG_okloC4urm53zm55yB0SPAJwYKcYox5LJkkZxRjKbSkW6hDOKMxVlxuo84G2EV7Iby0KyWadRDtz6BMPUTVNDj_Dk1elVGVRc3MRb38ORrkde18NImIpPzn65sbvI92MiiCO1jPLnocXjz0r-LR7eV1_3wUJ8zgJk4ld1Q4KrOEKCU0GMNTJVIpkkxN1VQQSNsncGaIAqeNBAbSaAIOlAQtWBcdr3xrX70tXGjsPA-JKwooXbUIlmLGBWemBekKTHwVgneZrX0-B_9pCbbLeuwyvV2mt3_1tKKjtTuEBIrMQ5nk4V-puRZEsJaLV1weGvexuYN_tVIxJazGY3szvL8b9J7GdsJ-AcM0cTU</recordid><startdate>20070201</startdate><enddate>20070201</enddate><creator>Iaria, R.</creator><creator>Lavagetto, G.</creator><creator>D'Aí, A.</creator><creator>Di Salvo, T.</creator><creator>Robba, N. 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R.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Chandra observation of the Big Dipper X 1624–490</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2007-02-01</date><risdate>2007</risdate><volume>463</volume><issue>1</issue><spage>289</spage><epage>295</epage><pages>289-295</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><coden>AAEJAF</coden><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 $\ion{Ca}{xx}$. We confirm the presence of the $\ion{Fe}{xxv}$ Kα and $\ion{Fe}{xxvi}$ Kα absorption lines with a larger accuracy with respect to a previous XMM observation. 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| ispartof | Astronomy and astrophysics (Berlin), 2007-02, Vol.463 (1), p.289-295 |
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| source | EDP Sciences; EZB Electronic Journals Library; EDP Sciences - Revues - Licences nationales - accès par la plateforme ISTEX |
| subjects | accretion accretion disks Astronomy Earth, ocean, space Exact sciences and technology stars: individual: X 1624–490 stars: neutron X-rays: binaries X-rays: general X-rays: stars |
| title | Chandra observation of the Big Dipper X 1624–490 |
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