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PSR J0348+0432 is a neutron star in a binary system with a white dwarf. It was discovered in 2007 with the Green Bank Telescope in a drift-scan survey.〔 In 2013, a mass measurement for this neutron star was announced: .〔 This measurement was done with a combination of radio timing and precise spectroscopy of the white dwarf companion. This is slightly higher, but statistically indistinguishable, from the mass of PSR J1614-2230, which was measured using the Shapiro delay.〔 This measurement confirmed the existence of such massive neutron stars using a different measuring technique. The notable feature of this binary pulsar is its combination of high neutron star mass and short orbital period: 2 hours and 27 minutes. This allowed a measurement of the orbital decay due to the emission of gravitational waves, as observed for PSR B1913+16 and PSR J0737-3039. ==Background== (詳細はPulsars were discovered in 1967 by Jocelyn Bell and her adviser Antony Hewish using the Interplanetary Scintillation Array.〔 Franco Pacini and Thomas Gold quickly put forth the idea that pulsars are highly magnetized rotating neutron stars, which form as a result of a supernova at the end of the life of stars more massive than about 10 times the mass of the Sun ().〔〔 The radiation emitted by pulsars is caused by interaction of the plasma surrounding the neutron star with its rapidly rotating magnetic field. This interaction leads to emission "in the pattern of a rotating beacon," as emission escapes along the magnetic poles of the neutron star.〔 The "rotating beacon" property of pulsars arises from the misalignment of their magnetic poles with their rotational poles. Historically, pulsars have been discovered at radio wavelengths where emission is strong, but space telescopes that operate in the gamma ray wavelengths have also discovered pulsars. 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「PSR J0348+0432」の詳細全文を読む スポンサード リンク
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