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Prog. Theor. Phys. Vol. 81 No. 5 (1989) pp. 1006-1020

[ Full Text PDF : FREE ACCESS (868K) ]

Binary Sub-Millisecond Pulsar and Rotating Core Collapse Model for SN1987A

Takashi Nakamura

National Laboratory for High Energy Physics, Tsukuba 305

(Received March 3, 1989)

Abstract:

The recent discovery of a binary sub-millisecond pulsar in SN1987A strongly suggests that the rotation was important in the core collapse of the progenitor of SN1987A. The observed period of the pulsar 0.5079680 ms is close to the maximum rotation of the neutron star. The periodic modulation of the pulse period with 8 hours suggests the existence of the companion with an almost circular orbit. The mass of the companion is either ∼1.4 M⊙ (face-on) or ∼10-3 M⊙ (edge-on) with the semi-major axis of ∼2 ×1011 cm. In either case, if the companion has existed before the supernova explosion, it is hard to understand why the companion has a circular ortbit. The formation of the companion after the bounce of the core is proposed. If the angular momentum of the pre-supernova core is greater than ∼6 ×1049 cgs, the core fragments and a binary proto neutron star is formed. As the separation of two neutron stars decreases in several seconds, the larger mass neutron star begins to accrete the matter of the smaller mass neutron star. The sub-millisecond period of the pulsar is the consequence of the accretion of matter with the angular momentum ∼1049 cgs. Due to the tidal disruption at the end of the accretion, the system consists of a central neutron star and a rotating thin disk. Similar to the formation of planets in the solar nebula, a Jupiter-like secondary of mass ∼10-3 M⊙ with a circular orbit may be formed within a year at separation of ∼1011 cm. A possible detection of the gravitational radiation from the sub-millisecond pulsar and a possible origin of gamma ray bursters are also demonstrated.


URL : http://ptp.ipap.jp/link?PTP/81/1006/
DOI : 10.1143/PTP.81.1006

[ Full Text PDF : FREE ACCESS (868K) ] Citation:

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Citing Article(s) :

  1. Progress of Theoretical Physics Vol. 82 No. 3 (1989) pp. 535-554 :
    Gravitational Radiation from Coalescing Binary Neutron Stars. I
    Ken-ichi Oohara and Takashi Nakamura
  2. Progress of Theoretical Physics Vol. 83 No. 3 (1990) pp. 499-521 :
    Static and Dynamical Properties of Neutron Stars with Combined π0-πc Condensation
    Takumi Muto and Toshitaka Tatsumi
  3. Progress of Theoretical Physics Vol. 85 No. 2 (1991) pp. 175-180 :
    Effect of Pion Condensation on Keplerian Angular Frequency of Rotating Neutron Stars
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  4. Progress of Theoretical Physics Vol. 86 No. 1 (1991) pp. 73-88 :
    Gravitational Radiation from Coalescing Binary Neutron Stars. IV
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  5. Progress of Theoretical Physics Vol. 87 No. 4 (1992) pp. 879-890 :
    Some Comments on the Origin of Gamma Ray Bursts
    Takashi Nakamura, Noriaki Shibazaki, Yoshio Murakami and Atsumasa Yoshida
  6. Progress of Theoretical Physics Vol. 94 No. 6 (1995) pp. 1001-1010 :
    (C + O) Star-Neutron Star Close Binary System Is a Progenitor of Soft Gamma-Ray Repeater?
    Hitoshi Hanami, Takashi Nakamura and Toshio Murakami
  7. Progress of Theoretical Physics Supplement No.112 (1993) pp. 221-275 :
    Chapter VIII. Implications of Various Hadron Phases to Neutron Star Phenomena
    Takumi Muto, Tatsuyuki Takatsuka, Ryozo Tamagaki and Toshitaka Tatsumi

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