本文選題：銀心 + 脈沖星-黑洞雙星　； 參考：《中國科學(xué)技術(shù)大學(xué)》2014年碩士論文

【摘要】：脈沖星是宇宙中最精確的時鐘,其信號周期的精確度能夠超過原子鐘。1979年,Hulse和Taylor發(fā)現(xiàn)了脈沖雙星PSR B1913+16(脈沖星帶有一個中子星伴星),該系統(tǒng)軌道周期的衰減率與廣義相對論預(yù)言的由引力輻射造成的軌道衰減相符合,這間接驗證了引力波的存在。到目前為止,廣義相對論僅僅在弱場(例如太陽系)中被正確檢驗,脈沖雙星的發(fā)現(xiàn)為未來在強場中精確檢驗廣義相對論提供了可能。若脈沖星的伴星是一個黑洞,那么引力效應(yīng)將更加顯著,我們可以利用脈沖星精準(zhǔn)的脈沖到達時間作為研究強引力物理和黑洞性質(zhì)的探針。 本文研究的對象是脈沖星圍繞星系中心超大質(zhì)量黑洞做軌道運動的雙星系統(tǒng)。脈沖星發(fā)出的脈沖在到達地球的過程中,如果途徑黑洞附近,會被強引力場彎曲,原則上可以通過觀測接收到的脈沖來研究黑洞和強引力場的性質(zhì)。我們以圍繞銀河系中心超大質(zhì)量黑洞Sgr A*做圓周運動的脈沖星為例,分析了強引力場對脈沖路徑的影響和脈沖到達時間的延遲。結(jié)果表明,脈沖軌跡和時延敏感依賴于觀測者的觀測傾角。觀測角越大,強引力場效應(yīng)就越顯著。相比于黑洞的引力質(zhì)量,黑洞自旋對結(jié)果的影響較小；當(dāng)觀測者偏離脈沖星軌道平面較大(即觀測角較小時),黑洞自旋造成的效應(yīng)明顯變小；因此,需要借助高精度和靈敏度的望遠鏡來探究黑洞自旋的影響。隨著大型射電望遠鏡FAST、SKA等的建成使用,我們有理由相信,發(fā)現(xiàn)更多、距離Sgr A*更近的脈沖星指日可待。
[Abstract]:Pulsars are the most accurate clocks in the universe, In 1979, Hulse and Taylor discovered the pulsars PSR B191316 (pulsar with a neutron star companion), the decay rate of the orbital period of the system and the gravitational radiation predicted by the general relativity. The resulting orbital decay is consistent, This indirectly verifies the existence of gravitational waves. So far, general relativity has only been correctly tested in weak fields (such as the solar system), and the discovery of pulsating binary stars has made it possible to accurately test general relativity in strong fields in the future. If the pulsar's companion is a black hole, the gravitational effect will be more significant. We can use the pulsar's precise pulse arrival time as a probe to study the properties of strong gravitational physics and black hole. The object of this paper is a binary system of pulsars orbiting supermassive black holes in the center of galaxies. In the process of reaching the earth the pulsars will be bent by the strong gravitational field if the path is near the black hole. In principle the properties of the black hole and the strong gravitational field can be studied by observing the received pulse. In this paper, the influence of strong gravitational field on the pulse path and the delay of the arrival time of the pulse are analyzed by taking the pulsar with circular motion around the supermassive black hole Sgr A * in the center of the Milky way as an example. The results show that the pulse trajectory and time delay sensitivity depend on the observational inclination. The larger the observation angle, the more significant the strong gravitational field effect is. Compared with the gravitational mass of the black hole, the spin of the black hole has less effect on the result. When the observer deviates from the plane of the pulsar orbit (that is, the observation angle is small), the effect caused by the spin of the black hole is obviously smaller. High precision and sensitivity telescopes are needed to explore the effects of black hole spin. With the completion and use of the large radio telescope FASTX SKA, we have reason to believe that more pulsars closer to Sgr A * are within reach.
【學(xué)位授予單位】：中國科學(xué)技術(shù)大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2014
【分類號】：P145.6;P145.8

【共引文獻】

相關(guān)期刊論文 前1條

1 董宏偉;;黑洞質(zhì)量分布[J];山西煤炭管理干部學(xué)院學(xué)報;2014年01期

相關(guān)博士學(xué)位論文 前1條

1 彭志欣;活動星系核發(fā)射線的物理性質(zhì)[D];南京大學(xué);2013年

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本文編號：2102719