PSR J1930-1852: a pulsar in the widest known orbit around another neutron star
| Autor: | Swiggum, J. K., Rosen, R., McLaughlin, M. A., Lorimer, D. R., Heatherly, S., Lynch, R., Scoles, S., Hockett, T., Filik, E., Marlowe, J. A., Barlow, B. N., Weaver, M., Hilzendeger, M., Ernst, S., Crowley, R., Stone, E., Miller, B., Nunez, R., Trevino, G., Doehler, M., Cramer, A., Yencsik, D., Thorley, J., Andrews, R., Laws, A., Wenger, K., Teter, L., Snyder, T., Dittmann, A., Gray, S., Carter, M., McGough, C., Dydiw, S., Pruett, C., Fink, J., Vanderhout, A. |
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| Rok vydání: | 2015 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1088/0004-637X/805/2/156 |
| Popis: | In the summer of 2012, during a Pulsar Search Collaboratory workshop, two high-school students discovered J1930$-$1852, a pulsar in a double neutron star (DNS) system. Most DNS systems are characterized by short orbital periods, rapid spin periods and eccentric orbits. However, J1930$-$1852 has the longest spin period ($P_{\rm spin}\sim$185 ms) and orbital period ($P_{\rm b}\sim$45 days) yet measured among known, recycled pulsars in DNS systems, implying a shorter than average and/or inefficient recycling period before its companion went supernova. We measure the relativistic advance of periastron for J1930$-$1852, $\dot{\omega}=0.00078$(4) deg/yr, which implies a total mass (M$_{\rm{tot}}=2.59$(4) M$_{\odot}$) consistent with other DNS systems. The $2\sigma$ constraints on M$_{\rm{tot}}$ place limits on the pulsar and companion masses ($m_{\rm p}<1.32$ M$_{\odot}$ and $m_{\rm c}>1.30$ M$_{\odot}$ respectively). J1930$-$1852's spin and orbital parameters challenge current DNS population models and make J1930$-$1852 an important system for further investigation. Comment: 8 pages, 6 figures |
| Databáze: | arXiv |
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