Further Evidence for the Bimodal Distribution of Neutron Star Masses
We use a collection of 14 well-measured neutron star masses to strengthen the case that a substantial fraction of these neutron stars was formed via electron-capture supernovae (SNe) as opposed to Fe-core collapse SNe. The e-capture SNe are characterized by lower resultant gravitational masses and s...
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| Format: | Journal article |
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2010
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| _version_ | 1797096193635909632 |
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| author | Schwab, J Podsiadlowski, P Rappaport, S |
| author_facet | Schwab, J Podsiadlowski, P Rappaport, S |
| author_sort | Schwab, J |
| collection | OXFORD |
| description | We use a collection of 14 well-measured neutron star masses to strengthen the case that a substantial fraction of these neutron stars was formed via electron-capture supernovae (SNe) as opposed to Fe-core collapse SNe. The e-capture SNe are characterized by lower resultant gravitational masses and smaller natal kicks, leading to lower orbital eccentricities when the e-capture SN has led to the formation of the second neutron star in a binary system. Based on the measured masses and eccentricities, we identify four neutron stars, which have a mean post-collapse gravitational mass of ~1.25 solar masses, as the product of e-capture SNe. We associate the remaining ten neutron stars, which have a mean mass of 1.35 solar masses, with Fe-core collapse SNe. If the e-capture supernova occurs during the formation of the first neutron star, then this should substantially increase the formation probability for double neutron stars, given that more systems will remain bound with the smaller kicks. However, this does not appear to be the case for any of the observed systems, and we discuss possible reasons for this. |
| first_indexed | 2024-03-07T04:38:36Z |
| format | Journal article |
| id | oxford-uuid:d0d70423-5636-4f99-9fa9-7b5ec74086f9 |
| institution | University of Oxford |
| last_indexed | 2024-03-07T04:38:36Z |
| publishDate | 2010 |
| record_format | dspace |
| spelling | oxford-uuid:d0d70423-5636-4f99-9fa9-7b5ec74086f92022-03-27T07:52:52ZFurther Evidence for the Bimodal Distribution of Neutron Star MassesJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:d0d70423-5636-4f99-9fa9-7b5ec74086f9Symplectic Elements at Oxford2010Schwab, JPodsiadlowski, PRappaport, SWe use a collection of 14 well-measured neutron star masses to strengthen the case that a substantial fraction of these neutron stars was formed via electron-capture supernovae (SNe) as opposed to Fe-core collapse SNe. The e-capture SNe are characterized by lower resultant gravitational masses and smaller natal kicks, leading to lower orbital eccentricities when the e-capture SN has led to the formation of the second neutron star in a binary system. Based on the measured masses and eccentricities, we identify four neutron stars, which have a mean post-collapse gravitational mass of ~1.25 solar masses, as the product of e-capture SNe. We associate the remaining ten neutron stars, which have a mean mass of 1.35 solar masses, with Fe-core collapse SNe. If the e-capture supernova occurs during the formation of the first neutron star, then this should substantially increase the formation probability for double neutron stars, given that more systems will remain bound with the smaller kicks. However, this does not appear to be the case for any of the observed systems, and we discuss possible reasons for this. |
| spellingShingle | Schwab, J Podsiadlowski, P Rappaport, S Further Evidence for the Bimodal Distribution of Neutron Star Masses |
| title | Further Evidence for the Bimodal Distribution of Neutron Star Masses |
| title_full | Further Evidence for the Bimodal Distribution of Neutron Star Masses |
| title_fullStr | Further Evidence for the Bimodal Distribution of Neutron Star Masses |
| title_full_unstemmed | Further Evidence for the Bimodal Distribution of Neutron Star Masses |
| title_short | Further Evidence for the Bimodal Distribution of Neutron Star Masses |
| title_sort | further evidence for the bimodal distribution of neutron star masses |
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