李向东
研究方向为高能天体物理:X射线双星的时变特性;X射线双星的形成和演化;中子星物态和奇异星的观测对应体;反常X射线脉冲星和软γ射线复现源;中子星磁场和吸积盘的相互作用;双星系统中吸积盘的不稳定性。
个性化签名
- 姓名:李向东
- 目前身份:
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学术头衔:
博士生导师
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学科领域:
天体物理学
- 研究兴趣:研究方向为高能天体物理:X射线双星的时变特性;X射线双星的形成和演化;中子星物态和奇异星的观测对应体;反常X射线脉冲星和软γ射线复现源;中子星磁场和吸积盘的相互作用;双星系统中吸积盘的不稳定性。
李向东,1969年3月生,理学博士、教授。1995年7月毕业于南京大学天文系后留系任教。现任系主任、华东天文与天体物理中心主任。1998年被评为南京大学中青年骨干教师。
研究方向为高能天体物理:X射线双星的时变特性;X射线双星的形成和演化;中子星物态和奇异星的观测对应体;反常X射线脉冲星和软γ射线复现源;中子星磁场和吸积盘的相互作用;双星系统中吸积盘的不稳定性。
主要成果包括系统提出Ia型超新星的两类前身星及其与超软X射线源之间的联系、利用X射线双星的观测资料证认奇异星的候选天体和双星系统中的超磁星候选天体、改进和发展中子星磁场与吸积盘相互作用的理论模型和研究低质量X射线双星中吸积盘的热不稳定性条件及其观测证据等。1998年获教育部科技进步一等奖,1999年获国家自然科学三等奖。
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李向东, X.-D. Li, and E.P.J. van den Heuvel
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-1年11月30日
The discovery of supersoft X-ray sources, described as massive white dwarfs burning accreted matter from their (more massive) companions, opens a new channel to type Ia supernovae (SNe Ia). According to conventional binary evolutionary theory, if the mass ratio of the donor to the white dwarf exceeds a critical value, the mass transfer becomes unstable, and a common envelope will be formed. However, recent calculations by Hachisu, Kato & Nomoto (1996) suggest a strongwind to stabilize the mass transfer when the mass transfer rate is higher than a certain value. Adopting the strong wind assumption, we have performed evolutionary calculations of white dwarf binaries, in which mass transfer occurs through Rochelobe overflow, to search for the progenitors of SNe Ia. We ndthat there are two types of systems that can produce SNe Ia. One is close binaries with ~2 to ~3.5 main-sequence or subgiant companions, and the initial orbital period of several tenth of a day to several days. The other is wide binaries with low-mass (~1M) red giant companions and long initial orbital period (tens to hundreds of days). The derived birth rate of SNe Ia in the Galaxy is roughly consistent with the observed one.
binaries, close-stars, mass loss-supernovae, general
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【期刊论文】Could 2S 0114+650 be a magnetar?
李向东, X.-D. Li, and E. P.J. van den Heuvel
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-1年11月30日
We investigate the spin evolution of the binary X-ray pulsar 2S 0114+650, which possesses the slowest known spin period of ~2.7 hours. We argue that, to interpret such long spin period, the magnetic field strength of this pulsar must be initially >~10 14 G, that is, it was born as a magnetar. Since the pulsar currently has a normal magnetic field ~1012 G, our results present support for magnetic field decay predicted by the magnetar model.
binaries, close-pulsars, individual, 2S 0114+, 650-stars, neutron-X-ray, stars
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【期刊论文】Is SAX J1808.4-3658 A Strange Star?
李向东, X.-D. Li, I. Bombaci, M. Dey, J. Dey, E.P.J. van den Heuvel
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-1年11月30日
One of the most important questions in the study of compact objects is the nature of pulsars, including whether they are composed of β-stable nuclear matter or strange quark matter. Obser-vations of the newly discovered millisecond X-ray pulsar SAX J1808.4-3658 with the Rossi X-Ray Timing Explorer place firm constraint on the radius of the compact star. Comparing the mass-radius relation of SAX J1808.4-3658 with the theoretical mass-radius relation for neutron stars and for strange stars, we find that a strange star model is more consistent with SAX J1808.4-3658, and suggest that it is a likely strange star candidate.
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