Formation of Sub-millisecond Pulsars and Possibility of Detection

Details Formation of Sub-millisecond Pulsars and Possibility of Detection Formation of Sub-millisecond Pulsars and Possibility of Detection

2009-07-15

arxiv.org/abs/0907.2611v1

Mon. Not. R. Astron. Soc. 399, 1587-1596 (2009)

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

10 pages, 4 figures, 4 tables, accepted by MNRAS

Scientific paper

10.1111/j.1365-2966.2009.15373.x

Pulsars have been recognized as normal neutron stars, but sometimes argued as quark stars. {\it Sub-millisecond pulsars, if detected, would play an essential and important role in distinguishing quark stars from neutron stars.} We focus on the formation of such sub-millisecond pulsars in this paper. A new approach to form a sub-millisecond pulsar (quark star) via accretion induced collapse (AIC) of a white dwarf is investigated here. Under this AIC process, we found that: (1) almost all the newborn quark stars could have an initial spin period of $\sim 0.1$ ms; (2) the nascent quark stars (even with a low mass) have sufficiently high spin-down luminosity and satisfy the conditions for pair production and sparking process to be as sub-millisecond radio pulsars; (3) in most cases, the timescales of newborn quark stars in the phase of spin period $< 1$ (or $<0.5$) ms can be long enough to be detected. As a comparison, an accretion spin-up process (for both neutron and quark stars) is also investigated. It is found that, quark stars formed through AIC process can have shorter periods ($\leq$ 0.5 ms); while the periods of neutron stars formed in accretion spin-up process must be longer than 0.5ms. Thus if a pulsar with a period less than 0.5 ms can be identified in the future, it should be a quark star.

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