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Parkes observations for project P1000 semester 2018OCTS_10
Hot subdwarf (sdB) stars are core-helium burning stars with thin hydrogen envelopes and masses around 0.5 Msun. A large fraction of sdBs are members of short-period binaries with periods below a few days. Orbital shrinkage through a common envelope phase is the only likely formation channel for such short-period sdB binaries.
Although most of th... moree companions are low mass main sequence stars or white dwarfs, one proposed evolutionary channel produces an sdB with a recycled pulsar companion where the pulsar forms after two common envelope phases and a short X-ray binary phase. Theoretical models predict that about 1% of the compact sdB binaries should have pulsar companions.
So far no pulsar companion to an sdB has yet been detected unambiguously whereas six candidates have been identified. Here we propose 13.5 hrs of observing time to conduct a deep search for radio pulsars around four candidate sdB+pulsar systems which are accessible with Parkes. A detection would (a) be the first time a pulsar bound to an sdB star has been detected, confirming the efficacy of the predicted binary-evolution channel; and (b) allow for an accurate estimate of the sdB mass, testing models for these enigmatic stars. less
Astronomical and Space Sciences not elsewhere classified
01 Oct 2018
01 Apr 2019
compact binaries and/or black-holes
Creative Commons Attribution 4.0 International Licence
Kupfer, Thomas; Ravi, Vikram; Geier, Stephan (2018): Parkes observations for project P1000 semester 2018OCTS_10. v1. CSIRO. Data Collection.
All Rights (including copyright) CSIRO 2018.
The metadata and files (if any) are available to the public.
Australia Telescope National Facility
P1000 - A deep search for radio pulsars around hot subdwarf stars in compact binaries
Hot subdwarf stars are core-helium burning stars with thin hydrogen layers. They have masses around half the mass of the sun. Mass transfer with a companion star is required to remove a large fraction of the hydrogen envelope and indeed a large fraction of these objects have a close companion with orbital periods of less than a few days. Most of th... moree companions are low-mass stars or white dwarfs. However, theoretical models predict that about 1% of the hot subdwarf stars should host a neutron star companion. So far no neutron star companion to a hot subdwarf has yet been detected unambiguously whereas six candidates have been identified. These systems seem to have a companion mass which is potentially high enough for a neutron star. Here, we conduct a deep search in four of the candidates to search for the first known neutron star around a hot subdwarf star. less
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