Spin‐down rate and inferred dipole magnetic field of the soft gamma‐ray repeater SGR 1627–41
Identifieur interne : 007D73 ( Main/Exploration ); précédent : 007D72; suivant : 007D74Spin‐down rate and inferred dipole magnetic field of the soft gamma‐ray repeater SGR 1627–41
Auteurs : P. Esposito [Italie] ; M. Burgay [Italie] ; A. Possenti [Italie] ; R. Turolla [Italie, Royaume-Uni] ; S. Zane [Royaume-Uni] ; A. De Luca [Italie] ; A. Tiengo [Italie] ; G. L. Israel [Italie] ; F. Mattana [France] ; S. Mereghetti [Italie] ; M. Bailes [Australie] ; P. Romano [Italie] ; D. Götz [France] ; N. Rea [Pays-Bas, Espagne]Source :
- Monthly Notices of the Royal Astronomical Society: Letters [ 1745-3925 ] ; 2009-10-11.
English descriptors
- KwdEn :
- Archival, Archival data, Archival radio data, Astron, Axps, Burst activation, Cambridge univ, Camilo, Camilo sarkissian, Cent duty cycle, Chandra, Chandra center, Chandra data, Chandra observatory, Cordes lazio, Density limit, Energy range, Esposito, Gavriil, Journal compilation, Long observation, Luminosity, Magnetar, Magnetar nature, Magnetar rates, Magnetar sources, Magnetars, Mereghetti, Mnras, Neutron, Neutron star, Ordinary radio pulsars, Parkes radio telescope, Pulsar, Radio emission, Radio magnetars, Radio properties, Same class, Sgrs, Soft repeater, Spie conf, Thermal component, Timing properties, Variability ranges, Vertical bars.
- Teeft :
- Archival, Archival data, Archival radio data, Astron, Axps, Burst activation, Cambridge univ, Camilo, Camilo sarkissian, Cent duty cycle, Chandra, Chandra center, Chandra data, Chandra observatory, Cordes lazio, Density limit, Energy range, Esposito, Gavriil, Journal compilation, Long observation, Luminosity, Magnetar, Magnetar nature, Magnetar rates, Magnetar sources, Magnetars, Mereghetti, Mnras, Neutron, Neutron star, Ordinary radio pulsars, Parkes radio telescope, Pulsar, Radio emission, Radio magnetars, Radio properties, Same class, Sgrs, Soft repeater, Spie conf, Thermal component, Timing properties, Variability ranges, Vertical bars.
Abstract
Using Chandra data taken in 2008 June, we detected pulsations at 2.594 39(4) s in the soft gamma‐ray repeater SGR 1627−41. This is the second measurement of the source spin period and allows us to derive for the first time a long‐term spin‐down rate of (1.9 ± 0.4) × 10−11 s s−1. From this value, we infer for SGR 1627−41 a characteristic age of ∼2.2 kyr, a spin‐down luminosity of ∼4 × 1034 erg s−1 (one of the highest among sources of the same class), and a surface dipole magnetic field strength of ∼2 × 1014 G. These properties confirm the magnetar nature of SGR 1627−41; however, they should be considered with caution since they were derived on the basis of a period derivative measurement made using two epochs only, and magnetar spin‐down rates are generally highly variable. The pulse profile, double‐peaked and with a pulsed fraction of 13 ± 2 per cent in the 2–10 keV range, closely resembles that observed by XMM–Newton in 2008 September. Having for the first time a timing model for this soft gamma‐ray repeater (SGR), we also searched for a pulsed signal in archival radio data collected with the Parkes radio telescope 9 months after the previous X‐ray outburst. No evidence for radio pulsations was found, down to a luminosity level ∼10–20 times fainter (for a 10 per cent duty cycle and a distance of 11 kpc) than the peak luminosity shown by the known radio magnetars.
Url:
- https://api.istex.fr/document/A597AC9DA5E49198B13E934B81A7CDF03BA1E0E0/fulltext/pdf
- https://api.istex.fr/document/3786EE8E1A46BEBBB3EBCB885CF5BC7DE6884A9A/fulltext/pdf
DOI: 10.1111/j.1745-3933.2009.00723.x
Affiliations:
- Australie, Espagne, France, Italie, Pays-Bas, Royaume-Uni
- Angleterre, Catalogne, Grand Londres, Hollande-Septentrionale, Vénétie, Île-de-France
- Amsterdam, Barcelone, Gif sur Yvette, Londres, Padoue, Paris
- University College de Londres, Université d'Amsterdam, Université de Padoue
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Le document en format XML
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Rea</name><affiliation wicri:level="4"><country xml:lang="fr" wicri:curation="lc">Pays-Bas</country><wicri:regionArea>University of Amsterdam, Astronomical Institute Anton Pannekoek, Kruislaan 403, 1098 SJ Amsterdam</wicri:regionArea><orgName type="university">Université d'Amsterdam</orgName><placeName><settlement type="city">Amsterdam</settlement><region>Hollande-Septentrionale</region></placeName></affiliation><affiliation wicri:level="1"><country xml:lang="fr">Espagne</country><wicri:regionArea>CSIC – Institut d'Estudis Espacials de Catalunya, Campus UAB, Fac. Ciències, Torre C5 parell 2, 08193 Barcelona</wicri:regionArea><placeName><settlement type="city">Barcelone</settlement><region nuts="2" type="region">Catalogne</region></placeName></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society: Letters</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LETTERS</title><idno type="ISSN">1745-3925</idno><idno type="eISSN">1745-3933</idno><imprint><biblScope unit="vol">399</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="L44">L44</biblScope><biblScope unit="page" to="L48">L48</biblScope><biblScope unit="page-count">5</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2009-10-11">2009-10-11</date></imprint><idno type="ISSN">1745-3925</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">1745-3925</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Archival</term><term>Archival data</term><term>Archival radio data</term><term>Astron</term><term>Axps</term><term>Burst activation</term><term>Cambridge univ</term><term>Camilo</term><term>Camilo sarkissian</term><term>Cent duty cycle</term><term>Chandra</term><term>Chandra center</term><term>Chandra data</term><term>Chandra observatory</term><term>Cordes lazio</term><term>Density limit</term><term>Energy range</term><term>Esposito</term><term>Gavriil</term><term>Journal compilation</term><term>Long observation</term><term>Luminosity</term><term>Magnetar</term><term>Magnetar nature</term><term>Magnetar rates</term><term>Magnetar sources</term><term>Magnetars</term><term>Mereghetti</term><term>Mnras</term><term>Neutron</term><term>Neutron star</term><term>Ordinary radio pulsars</term><term>Parkes radio telescope</term><term>Pulsar</term><term>Radio emission</term><term>Radio magnetars</term><term>Radio properties</term><term>Same class</term><term>Sgrs</term><term>Soft repeater</term><term>Spie conf</term><term>Thermal component</term><term>Timing properties</term><term>Variability ranges</term><term>Vertical bars</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Archival</term><term>Archival data</term><term>Archival radio data</term><term>Astron</term><term>Axps</term><term>Burst activation</term><term>Cambridge univ</term><term>Camilo</term><term>Camilo sarkissian</term><term>Cent duty cycle</term><term>Chandra</term><term>Chandra center</term><term>Chandra data</term><term>Chandra observatory</term><term>Cordes lazio</term><term>Density limit</term><term>Energy range</term><term>Esposito</term><term>Gavriil</term><term>Journal compilation</term><term>Long observation</term><term>Luminosity</term><term>Magnetar</term><term>Magnetar nature</term><term>Magnetar rates</term><term>Magnetar sources</term><term>Magnetars</term><term>Mereghetti</term><term>Mnras</term><term>Neutron</term><term>Neutron star</term><term>Ordinary radio pulsars</term><term>Parkes radio telescope</term><term>Pulsar</term><term>Radio emission</term><term>Radio magnetars</term><term>Radio properties</term><term>Same class</term><term>Sgrs</term><term>Soft repeater</term><term>Spie conf</term><term>Thermal component</term><term>Timing properties</term><term>Variability ranges</term><term>Vertical bars</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Using Chandra data taken in 2008 June, we detected pulsations at 2.594 39(4) s in the soft gamma‐ray repeater SGR 1627−41. This is the second measurement of the source spin period and allows us to derive for the first time a long‐term spin‐down rate of (1.9 ± 0.4) × 10−11 s s−1. From this value, we infer for SGR 1627−41 a characteristic age of ∼2.2 kyr, a spin‐down luminosity of ∼4 × 1034 erg s−1 (one of the highest among sources of the same class), and a surface dipole magnetic field strength of ∼2 × 1014 G. These properties confirm the magnetar nature of SGR 1627−41; however, they should be considered with caution since they were derived on the basis of a period derivative measurement made using two epochs only, and magnetar spin‐down rates are generally highly variable. The pulse profile, double‐peaked and with a pulsed fraction of 13 ± 2 per cent in the 2–10 keV range, closely resembles that observed by XMM–Newton in 2008 September. Having for the first time a timing model for this soft gamma‐ray repeater (SGR), we also searched for a pulsed signal in archival radio data collected with the Parkes radio telescope 9 months after the previous X‐ray outburst. No evidence for radio pulsations was found, down to a luminosity level ∼10–20 times fainter (for a 10 per cent duty cycle and a distance of 11 kpc) than the peak luminosity shown by the known radio magnetars.</div></front></TEI><affiliations><list><country><li>Australie</li><li>Espagne</li><li>France</li><li>Italie</li><li>Pays-Bas</li><li>Royaume-Uni</li></country><region><li>Angleterre</li><li>Catalogne</li><li>Grand Londres</li><li>Hollande-Septentrionale</li><li>Vénétie</li><li>Île-de-France</li></region><settlement><li>Amsterdam</li><li>Barcelone</li><li>Gif sur Yvette</li><li>Londres</li><li>Padoue</li><li>Paris</li></settlement><orgName><li>University College de Londres</li><li>Université d'Amsterdam</li><li>Université de Padoue</li></orgName></list><tree><country name="Italie"><noRegion><name sortKey="Esposito, P" sort="Esposito, P" uniqKey="Esposito P" first="P." last="Esposito">P. 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Possenti</name><name sortKey="Romano, P" sort="Romano, P" uniqKey="Romano P" first="P." last="Romano">P. Romano</name><name sortKey="Tiengo, A" sort="Tiengo, A" uniqKey="Tiengo A" first="A." last="Tiengo">A. Tiengo</name><name sortKey="Turolla, R" sort="Turolla, R" uniqKey="Turolla R" first="R." last="Turolla">R. Turolla</name></country><country name="Royaume-Uni"><region name="Angleterre"><name sortKey="Turolla, R" sort="Turolla, R" uniqKey="Turolla R" first="R." last="Turolla">R. Turolla</name></region><name sortKey="Zane, S" sort="Zane, S" uniqKey="Zane S" first="S." last="Zane">S. Zane</name></country><country name="France"><region name="Île-de-France"><name sortKey="Mattana, F" sort="Mattana, F" uniqKey="Mattana F" first="F." last="Mattana">F. Mattana</name></region><name sortKey="Gotz, D" sort="Gotz, D" uniqKey="Gotz D" first="D." last="Götz">D. Götz</name></country><country name="Australie"><noRegion><name sortKey="Bailes, M" sort="Bailes, M" uniqKey="Bailes M" first="M." last="Bailes">M. Bailes</name></noRegion></country><country name="Pays-Bas"><region name="Hollande-Septentrionale"><name sortKey="Rea, N" sort="Rea, N" uniqKey="Rea N" first="N." last="Rea">N. Rea</name></region></country><country name="Espagne"><region name="Catalogne"><name sortKey="Rea, N" sort="Rea, N" uniqKey="Rea N" first="N." last="Rea">N. Rea</name></region></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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