A transient I‐band excess in the optical spectrum of the accreting millisecond pulsar SAX J1808.4–3658
Identifieur interne : 009A52 ( Main/Exploration ); précédent : 009A51; suivant : 009A53A transient I‐band excess in the optical spectrum of the accreting millisecond pulsar SAX J1808.4–3658
Auteurs : J. G. Greenhill [Australie] ; A. B. Giles [Australie] ; C. Coutures [France]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2006-08-11.
Descripteurs français
- Pascal (Inist)
- Binaire RX, Contrepartie optique, Couleur, Disque accrétion, Emission RX, Instabilité, Intensité, Phase initiale, Pulsar milliseconde, Rayonnement non thermique, Rayonnement synchrotron, Satellite RXTE, Source RX binaire, Source RX cosmique, Source RX transitoire, Spectre optique, Sursaut RX, Sursaut RX type I, Transfert masse, Viscosité.
English descriptors
- KwdEn :
- Accreting, Accreting millisecond pulsar, Accreting millisecond pulsars, Accretion disc, Accretion disks, Binary, Binary X ray source, Burst source, Bvri, Bvri spectra, Canopus observatory, Chakrabarty, Chakrabarty morgan, Color, Colour, Colour indices, Colour temperature, Companion star, Cosmic x-ray sources, Discovery outburst, Early phase, Inner disc, Inner disc emission, Instability, Intensity, Interstellar extinction, Journal compilation, June, Light curves, Lled circles, Local standards, Lower panel, Mass transfer, Millisecond, Millisecond pulsar, Mnras, Nonthermal radiation, Optical burst, Optical bursts, Optical counterpart, Optical emission, Optical magnitudes, Optical spectra, Optical spectrum, Orbital modulation, Other colours, Outburst, Preliminary calculations, Primary outburst, Pulsar, Quiescent state, RXTE satellite, Reprocessed, Reprocessed radiation, Reprocessing, Same night, Same peak burst, Secondary outburst, Secondary outbursts, Several days, Solid angle, Solid lines, Spectral changes, Synchrotron, Synchrotron emission, Synchrotron radiation, Time dependence, Transient X ray source, Type I X ray burst, Upper limit, Upper panel, Viscosity, Viscosity change, Wang, Wijnands, X ray burst, X ray emission, X-ray binary stars.
- Teeft :
- Accreting, Accreting millisecond pulsar, Accreting millisecond pulsars, Accretion disc, Binary, Burst source, Bvri, Bvri spectra, Canopus observatory, Chakrabarty, Chakrabarty morgan, Colour, Colour indices, Colour temperature, Companion star, Discovery outburst, Early phase, Inner disc, Inner disc emission, Interstellar extinction, Journal compilation, June, Light curves, Lled circles, Local standards, Lower panel, Millisecond, Millisecond pulsar, Mnras, Optical burst, Optical bursts, Optical emission, Optical magnitudes, Optical spectra, Optical spectrum, Orbital modulation, Other colours, Outburst, Preliminary calculations, Primary outburst, Pulsar, Quiescent state, Reprocessed, Reprocessed radiation, Reprocessing, Same night, Same peak burst, Secondary outburst, Secondary outbursts, Several days, Solid angle, Solid lines, Spectral changes, Synchrotron, Synchrotron emission, Time dependence, Upper limit, Upper panel, Viscosity change, Wang, Wijnands.
Abstract
The optical counterpart of the transient, millisecond X‐ray pulsar SAX J1808.4–3658 was observed in four colours (BVRI) for five weeks during the 2005 June–July outburst. The optical fluxes declined by ∼2 mag during the first 16d and then commenced quasi‐periodic secondary outbursts, with time‐scales of several days, similar to those seen in 2000 and 2002. The broad‐band spectra derived from these measurements were generally consistent with emission from an X‐ray heated accretion disc. During the first 16d decline in intensity the spectrum became redder. We suggest that the primary outburst was initiated by a viscosity change driven instability in the inner disc and note the contrast with another accreting millisecond pulsar, XTE J0929−314, for which the spectrum becomes bluer during the decline. On the night of 2005 June 5 (HJD 245 3527) the I‐band flux was ∼0.45‐mag brighter than on the preceding or following nights whereas the BV and R bands showed no obvious enhancement. A type I X‐ray burst was detected by the Rossi X‐ray Timing Explorer spacecraft during this I‐band integration. It seems unlikely that reprocessed radiation from the burst was sufficient to explain the observed increase. We suggest that a major part of the I‐band excess was due to synchrotron emission triggered by the X‐ray burst. Several other significant short duration changes in V−I were detected. One occurred at about HJD 245 3546 in the early phase of the first secondary outburst and may be due to mass‐transfer instability or to another synchrotron emission event.
Url:
DOI: 10.1111/j.1365-2966.2006.10544.x
Affiliations:
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type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accreting</term><term>Accreting millisecond pulsar</term><term>Accreting millisecond pulsars</term><term>Accretion disc</term><term>Accretion disks</term><term>Binary</term><term>Binary X ray source</term><term>Burst source</term><term>Bvri</term><term>Bvri spectra</term><term>Canopus observatory</term><term>Chakrabarty</term><term>Chakrabarty morgan</term><term>Color</term><term>Colour</term><term>Colour indices</term><term>Colour temperature</term><term>Companion star</term><term>Cosmic x-ray sources</term><term>Discovery outburst</term><term>Early phase</term><term>Inner disc</term><term>Inner disc emission</term><term>Instability</term><term>Intensity</term><term>Interstellar extinction</term><term>Journal compilation</term><term>June</term><term>Light curves</term><term>Lled circles</term><term>Local standards</term><term>Lower panel</term><term>Mass transfer</term><term>Millisecond</term><term>Millisecond pulsar</term><term>Mnras</term><term>Nonthermal radiation</term><term>Optical burst</term><term>Optical bursts</term><term>Optical counterpart</term><term>Optical emission</term><term>Optical magnitudes</term><term>Optical spectra</term><term>Optical spectrum</term><term>Orbital modulation</term><term>Other colours</term><term>Outburst</term><term>Preliminary calculations</term><term>Primary outburst</term><term>Pulsar</term><term>Quiescent state</term><term>RXTE satellite</term><term>Reprocessed</term><term>Reprocessed radiation</term><term>Reprocessing</term><term>Same night</term><term>Same peak burst</term><term>Secondary outburst</term><term>Secondary outbursts</term><term>Several days</term><term>Solid angle</term><term>Solid lines</term><term>Spectral changes</term><term>Synchrotron</term><term>Synchrotron emission</term><term>Synchrotron radiation</term><term>Time dependence</term><term>Transient X ray source</term><term>Type I X ray burst</term><term>Upper limit</term><term>Upper panel</term><term>Viscosity</term><term>Viscosity change</term><term>Wang</term><term>Wijnands</term><term>X ray burst</term><term>X ray emission</term><term>X-ray binary stars</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Binaire RX</term><term>Contrepartie optique</term><term>Couleur</term><term>Disque accrétion</term><term>Emission RX</term><term>Instabilité</term><term>Intensité</term><term>Phase initiale</term><term>Pulsar milliseconde</term><term>Rayonnement non thermique</term><term>Rayonnement synchrotron</term><term>Satellite RXTE</term><term>Source RX binaire</term><term>Source RX cosmique</term><term>Source RX transitoire</term><term>Spectre optique</term><term>Sursaut RX</term><term>Sursaut RX type I</term><term>Transfert masse</term><term>Viscosité</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Accreting</term><term>Accreting millisecond pulsar</term><term>Accreting millisecond pulsars</term><term>Accretion disc</term><term>Binary</term><term>Burst source</term><term>Bvri</term><term>Bvri spectra</term><term>Canopus observatory</term><term>Chakrabarty</term><term>Chakrabarty morgan</term><term>Colour</term><term>Colour indices</term><term>Colour temperature</term><term>Companion star</term><term>Discovery outburst</term><term>Early phase</term><term>Inner disc</term><term>Inner disc emission</term><term>Interstellar extinction</term><term>Journal compilation</term><term>June</term><term>Light curves</term><term>Lled circles</term><term>Local standards</term><term>Lower panel</term><term>Millisecond</term><term>Millisecond pulsar</term><term>Mnras</term><term>Optical burst</term><term>Optical bursts</term><term>Optical emission</term><term>Optical magnitudes</term><term>Optical spectra</term><term>Optical spectrum</term><term>Orbital modulation</term><term>Other colours</term><term>Outburst</term><term>Preliminary calculations</term><term>Primary outburst</term><term>Pulsar</term><term>Quiescent state</term><term>Reprocessed</term><term>Reprocessed radiation</term><term>Reprocessing</term><term>Same night</term><term>Same peak burst</term><term>Secondary outburst</term><term>Secondary outbursts</term><term>Several days</term><term>Solid angle</term><term>Solid lines</term><term>Spectral changes</term><term>Synchrotron</term><term>Synchrotron emission</term><term>Time dependence</term><term>Upper limit</term><term>Upper panel</term><term>Viscosity change</term><term>Wang</term><term>Wijnands</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">The optical counterpart of the transient, millisecond X‐ray pulsar SAX J1808.4–3658 was observed in four colours (BVRI) for five weeks during the 2005 June–July outburst. The optical fluxes declined by ∼2 mag during the first 16d and then commenced quasi‐periodic secondary outbursts, with time‐scales of several days, similar to those seen in 2000 and 2002. The broad‐band spectra derived from these measurements were generally consistent with emission from an X‐ray heated accretion disc. During the first 16d decline in intensity the spectrum became redder. We suggest that the primary outburst was initiated by a viscosity change driven instability in the inner disc and note the contrast with another accreting millisecond pulsar, XTE J0929−314, for which the spectrum becomes bluer during the decline. On the night of 2005 June 5 (HJD 245 3527) the I‐band flux was ∼0.45‐mag brighter than on the preceding or following nights whereas the BV and R bands showed no obvious enhancement. A type I X‐ray burst was detected by the Rossi X‐ray Timing Explorer spacecraft during this I‐band integration. It seems unlikely that reprocessed radiation from the burst was sufficient to explain the observed increase. We suggest that a major part of the I‐band excess was due to synchrotron emission triggered by the X‐ray burst. Several other significant short duration changes in V−I were detected. One occurred at about HJD 245 3546 in the early phase of the first secondary outburst and may be due to mass‐transfer instability or to another synchrotron emission event.</div></front></TEI><affiliations><list><country><li>Australie</li><li>France</li></country><region><li>Île-de-France</li></region><settlement><li>Gif‐sur‐Yvette</li></settlement></list><tree><country name="Australie"><noRegion><name sortKey="Greenhill, J G" sort="Greenhill, J G" uniqKey="Greenhill J" first="J. G." last="Greenhill">J. G. Greenhill</name></noRegion><name sortKey="Giles, A B" sort="Giles, A B" uniqKey="Giles A" first="A. B." last="Giles">A. B. Giles</name><name sortKey="Giles, A B" sort="Giles, A B" uniqKey="Giles A" first="A. B." last="Giles">A. B. Giles</name><name sortKey="Greenhill, J G" sort="Greenhill, J G" uniqKey="Greenhill J" first="J. G." last="Greenhill">J. G. Greenhill</name></country><country name="France"><region name="Île-de-France"><name sortKey="Coutures, C" sort="Coutures, C" uniqKey="Coutures C" first="C." last="Coutures">C. Coutures</name></region></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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