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Titolo:
Where may ultrafast rotating neutron stars be hidden?
Autore:
Burderi, L; Possenti, A; DAntona, F; Di Salvo, T; Burgay, M; Stella, L; Menna, MT; Iaria, R; Campana, S; dAmico, N;
Indirizzi:
Osservatorio Astron Monteporzio, I-00127 Rome, Italy Osservatorio Astron Monteporzio Rome Italy I-00127 , I-00127 Rome, Italy Osservatorio Astron Bologna, I-40127 Bologna, Italy Osservatorio Astron Bologna Bologna Italy I-40127 I-40127 Bologna, Italy Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands Univ Amsterdam Amsterdam Netherlands NL-1098 SJ J Amsterdam, Netherlands Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands Ctr High Energy Astrophys Amsterdam Netherlands NL-1098 SJ , Netherlands Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy Univ Bologna Bologna Italy I-40127 imento Astron, I-40127 Bologna, Italy Univ Palermo, Dipartimento Sci Fis Astron, I-90123 Palermo, Italy Univ Palermo Palermo Italy I-90123 ci Fis Astron, I-90123 Palermo, Italy Osserv Astron Brera, I-23807 Merate, Italy Osserv Astron Brera Merate Italy I-23807 on Brera, I-23807 Merate, Italy
Titolo Testata:
ASTROPHYSICAL JOURNAL
fascicolo: 1, volume: 560, anno: 2001,
parte:, 2
pagine: L71 - L74
SICI:
0004-637X(20011010)560:1<L71:WMURNS>2.0.ZU;2-R
Fonte:
ISI
Lingua:
ENG
Soggetto:
X-RAY BINARIES; MILLISECOND PULSARS; EVOLUTION; PERIODS; SEARCH;
Keywords:
accretion, accretion disks; binaries : general; pulsars : general; stars : neutron; X-rays : general; X-rays : stars;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
33
Recensione:
Indirizzi per estratti:
Indirizzo: Burderi, L Osservatorio Astron Monteporzio, Via Frascati 33, I-00127 Rome,Italy Osservatorio Astron Monteporzio Via Frascati 33 Rome Italy I-00127
Citazione:
L. Burderi et al., "Where may ultrafast rotating neutron stars be hidden?", ASTROPHYS J, 560(1), 2001, pp. L71-L74

Abstract

The existence of ultrafast rotating neutron stars (spin period P less thanor similar to1 ms) is expected on the basis of current models for the secular evolution of interacting binaries, although they have not been detectedyet. Their formation depends on the quantity of matter accreted by the neutron star which, in turn, is limited by the mechanism of mass ejection fromthe binary. An efficient mass ejection can avoid the formation of ultrafast pulsars or their accretion-induced collapse to a black hole. We propose that significant reductions of the mass transfer rate may cause the switch-on of a radio pulsar phase, whose radiation pressure may be capable of ejecting out of the system most of the matter transferred by the companion. Thiscan prevent, for long orbital periods and if a sufficiently fast spin has been reached, any further accretion, even if the original transfer rate is restored, thus limiting the minimum spin period attainable by the neutron star. We show that close systems (orbital periods P-orb similar to 1 hr) arethe only possible hosts for ultrafast spinning neutron stars. This could explain why ultrafast radio pulsars have not been detected so far, as the detection of pulsars with very short spin periods in close systems is hampered, in current radio surveys, by strong Doppler modulation and computationallimitations.

ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 29/11/20 alle ore 15:39:07