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Transformation of a star into a planet in a millisecond pulsar binary
M Bailes1, S D Bates, V Bhalerao
1Centre for Astrophysics and Supercomputing and ARC Centre for All-Sky Astrophysics (CAASTRO), Swinburne University of Technology, Post Office Box 218 Hawthorn, VIC 3122, Australia. mbailes@swin.edu.au
Science (New York, N.Y.)
|August 27, 2011
Summary
Researchers discovered a solitary millisecond pulsar, PSR J1719-1438, is actually in a binary system. Its companion may be an ultralow-mass carbon white dwarf, offering clues to pulsar origins.
Area of Science:
- Astronomy and Astrophysics
- Compact Objects
- Neutron Stars
Background:
- Millisecond pulsars (MSPs) are rapidly rotating neutron stars, typically found in binary systems where accretion spins them up.
- A significant fraction (around 30%) of MSPs are solitary, posing a challenge to the standard formation model.
- Understanding the origin of solitary MSPs is crucial for a complete picture of stellar evolution.
Purpose of the Study:
- To investigate the nature and origin of the solitary millisecond pulsar PSR J1719-1438.
- To determine if PSR J1719-1438 is truly solitary or part of a binary system.
- To characterize the companion object and its implications for pulsar evolution.
Main Methods:
- Utilizing data from the Parkes 64-meter radio telescope survey.
- Performing timing analysis of the pulsar signal to detect orbital variations.
- Calculating the mass and density of the companion object based on orbital parameters.
Main Results:
- The millisecond pulsar PSR J1719-1438 was detected in a binary system with an orbital period of 2.2 hours.
- The companion's mass is comparable to Jupiter's mass.
- The companion's high density (minimum 23 g/cm³) suggests it is an ultralow-mass carbon white dwarf.
Conclusions:
- The discovery challenges the solitary nature of some MSPs and provides evidence for binary formation pathways.
- The companion's properties suggest a past as an ultracompact low-mass X-ray binary.
- This system offers insights into the extreme evolution of binary stars and the survival of companions during accretion phases.
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