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dc.contributor.authorKoch-Miramond, L
dc.contributor.authorHaas, M
dc.contributor.authorPantin, E
dc.contributor.authorPodsiadlowski, P
dc.contributor.authorNaylor, Tim
dc.contributor.authorSauvage, M
dc.date.accessioned2016-03-01T10:16:57Z
dc.date.issued2002-05-01
dc.description.abstractWe have searched for evidence of emission at 15 mum with ISOCAM and at 90 mum with ISOPHOT from dust orbiting six nearby pulsars, both in binaries and in isolation, located at distances between about 100 to 1000 pc. No emission was detected at any of the pulsar positions, and for the nearest pulsar J0108-1431 the 3 sigma ma upper limits on the flux density is about 66 mJy at 15 mum and 22.5 mJy at 90 mum. Upper limits on the masses of circumpulsar dust are inferred at a given temperature using a simple modelling of the radiated flux; they are compared to upper limits on orbiting mass obtained with the dust heating model of Foster & Fisher (\cite{For96}). These results suggest that it is unlikely that any of these pulsars have sufficiently massive, circumpulsar discs, out of which planets may form in the future. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands and the United Kingdom) and with the participation of ISAS and NASA.en_GB
dc.identifier.citationVol. 387, pp. 233 - 239en_GB
dc.identifier.doi10.1051/0004-6361:20020386
dc.identifier.urihttp://hdl.handle.net/10871/20294
dc.language.isoenen_GB
dc.publisherEDP Sciencesen_GB
dc.relation.urlhttp://adsabs.harvard.edu/abs/2002A%26A...387..233Ken_GB
dc.subjectinfrared: starsen_GB
dc.subjectplanetary systems: formationen_GB
dc.subjectstars: pulsars: generalen_GB
dc.subjectstars: circumstellar matteren_GB
dc.titleDetermination of limits on disc masses around six pulsars at 15 and 90 mumen_GB
dc.typeArticleen_GB
dc.date.available2016-03-01T10:16:57Z
dc.identifier.issn0004-6361
dc.descriptionThe final version of the article was published by EDP Sciences via http://dx.doi.org/10.1051/0004-6361:20020386. This version was deposited by the author in arxiv.orgen_GB
dc.identifier.eissn1432-0746
dc.identifier.journalAstronomy and Astrophysicsen_GB


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