本文選題：天體測(cè)量學(xué) + 脈沖星�。� 參考：《天文學(xué)報(bào)》2016年05期

【摘要】：脈沖星自轉(zhuǎn)參數(shù)是脈沖星最重要的參數(shù)之一,能反映脈沖星本身的物理性質(zhì).根據(jù)計(jì)時(shí)觀測(cè)所得的自轉(zhuǎn)參數(shù)除了包含脈沖星本身固有的部分,還受到幾何因素的影響,例如地球自轉(zhuǎn)參數(shù)、歲差章動(dòng)模型、行星歷表誤差、脈沖星相對(duì)于太陽(yáng)系質(zhì)心(solar system barycenter,SSB)的速度和加速度.通過(guò)分析脈沖星計(jì)時(shí)觀測(cè)模型,從而推導(dǎo)出這些因素與脈沖星自轉(zhuǎn)參數(shù)的關(guān)系,進(jìn)一步估計(jì)了這些因素對(duì)自轉(zhuǎn)參數(shù)影響的量級(jí)大小.在現(xiàn)有的觀測(cè)精度下,地球自轉(zhuǎn)參數(shù)和歲差章動(dòng)模型的誤差對(duì)計(jì)時(shí)觀測(cè)的影響可忽略,可以認(rèn)為脈沖星自轉(zhuǎn)參數(shù)不受其影響.行星歷表誤差對(duì)自轉(zhuǎn)參數(shù)的影響遠(yuǎn)小于自轉(zhuǎn)參數(shù)本身,同樣可以忽略.脈沖星相對(duì)于太陽(yáng)系質(zhì)心的視向速度影響到脈沖星周期,該影響比脈沖星本身周期約小4個(gè)量級(jí).值得注意的是,脈沖星橫向速度和脈沖星相對(duì)于太陽(yáng)系質(zhì)心的視向加速度對(duì)周期變率的影響不可忽略,特別是對(duì)于周期變率較小的毫秒脈沖星來(lái)說(shuō),這兩個(gè)因素的影響可能是脈沖星視周期變率中的主要成分.
[Abstract]:The rotation parameter of pulsar is one of the most important parameters of pulsar, which can reflect the physical properties of pulsar itself. In addition to the inherent part of the pulsar itself, the rotation parameters obtained according to the timing observations are also affected by geometric factors, such as the Earth rotation parameters, precession nutation model, and astrological errors. The velocity and acceleration of pulsars relative to the solar system's centroid system solar barycenter. By analyzing the pulsar timing observation model, the relationship between these factors and the pulsar rotation parameters is deduced, and the magnitude of the influence of these factors on the rotation parameters is further estimated. Under the present observation precision, the errors of the Earth rotation parameters and precession nutation model can be neglected, and the pulsar rotation parameters are not affected by the errors. The effect of the errors on the rotation parameters is much smaller than that on the rotation parameters, which can also be neglected. The pulsar period is affected by the apparent velocity of the pulsar relative to the center of mass of the solar system, which is about 4 orders of magnitude smaller than that of the pulsar itself. It is worth noting that the effects of the lateral velocity of pulsars and the apparent acceleration of pulsars relative to the center of mass of the solar system on the rate of periodic variability cannot be ignored, especially for millisecond pulsars with low rate of periodic variability. The effect of these two factors may be the main component of the pulsar apparent period variability.
【作者單位】： 中國(guó)科學(xué)院上海天文臺(tái);中國(guó)科學(xué)院大學(xué);
【基金】：國(guó)家自然科學(xué)基金項(xiàng)目(U1431117)資助
【分類號(hào)】：P145.6
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本文編號(hào)：1981891