Jiamusi pulsar observations II. Scintillations of ten pulsars

doi:10.1051/0004-6361/201833215

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	Jiamusi pulsar observations II. Scintillations of ten pulsars
	Wang, P. F.1,2,5; Han, J. L.2,4,5; Han, L.3; Zhang, J. H.1,3; Li, J. Q.1,3; Wang, C.2,5; Han, J.2; Wang, T.2,4; Gao, X. Y.2,5
刊名	ASTRONOMY & ASTROPHYSICS
	2018-10-26
卷号	618 页码:15
关键词	pulsars: general ISM: general
ISSN号	1432-0746
DOI	10.1051/0004-6361/201833215
英文摘要	Context. Pulsars scintillate. Dynamic spectra show brightness variation of pulsars in the time and frequency domain. Secondary spectra demonstrate the distribution of fluctuation power in the dynamic spectra. Aims. Dynamic spectra strongly depend on observational frequencies, but were often observed at frequencies lower than 1.5 GHz. Scintillation observations at higher frequencies help to constrain the turbulence feature of the interstellar medium over a wide frequency range and can detect the scintillations of more distant pulsars. Methods. Ten pulsars were observed at 2250 MHz (S-band) with the Jiamusi 66 m telescope to study their scintillations. Their dynamic spectra were first obtained, from which the decorrelation bandwidths and timescales of diffractive scintillation were then derived by autocorrelation. Secondary spectra were calculated by forming the Fourier power spectra of the dynamic spectra. Results. Most of the newly obtained dynamic spectra are at the highest frequency or have the longest time span of any published data for these pulsars. For PSRs B0540 + 23, B2324 + 60, and B2351 + 61, these were the first dynamic spectra ever reported. The frequency dependence of the scintillation parameters indicates that the intervening medium can rarely be ideally turbulent with a Kolmogorov spectrum. The thin-screen model worked well at S -band for the scintillation of PSR B1933 + 16. Parabolic arcs were detected in the secondary spectra of three pulsars, PSRs B0355 + 54, B0540 + 23, and B2154 + 40, all of which were asymmetrically distributed. The inverted arclets of PSR B0355 + 54 were seen to evolve along the main parabola within a continuous observing session of 12 h, from which the angular velocity of the pulsar was estimated. This was consistent with the measurement by very long baseline interferometry.
资助项目	National Natural Science Foundation of China[11403043] ; National Natural Science Foundation of China[11473034] ; National Natural Science Foundation of China[11873058] ; Young Researcher Grant of National Astronomical Observatories Chinese Academy of Sciences ; Key Research Program of the Chinese Academy of Sciences[QYZDJ-SSW-SLH021] ; strategic Priority Research Program of Chinese Academy of Sciences[XDB23010200] ; Open Fund of the State Key Laboratory of Astronautic Dynamics of China[2016ADL-DW0401] ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences
WOS关键词	LONG-TERM SCINTILLATION ; BASE-LINE ARRAY ; REFRACTIVE INTERSTELLAR SCINTILLATION ; DIFFRACTIVE SCINTILLATION ; DENSITY TURBULENCE ; DYNAMIC SPECTRA ; POWER SPECTRUM ; RADIO PULSARS ; VELOCITIES ; PLASMA
WOS研究方向	Astronomy & Astrophysics
语种	英语
出版者	EDP SCIENCES S A
WOS记录号	WOS:000448353500001
资助机构	National Natural Science Foundation of China ; National Natural Science Foundation of China ; Young Researcher Grant of National Astronomical Observatories Chinese Academy of Sciences ; Young Researcher Grant of National Astronomical Observatories Chinese Academy of Sciences ; Key Research Program of the Chinese Academy of Sciences ; Key Research Program of the Chinese Academy of Sciences ; strategic Priority Research Program of Chinese Academy of Sciences ; strategic Priority Research Program of Chinese Academy of Sciences ; Open Fund of the State Key Laboratory of Astronautic Dynamics of China ; Open Fund of the State Key Laboratory of Astronautic Dynamics of China ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Young Researcher Grant of National Astronomical Observatories Chinese Academy of Sciences ; Young Researcher Grant of National Astronomical Observatories Chinese Academy of Sciences ; Key Research Program of the Chinese Academy of Sciences ; Key Research Program of the Chinese Academy of Sciences ; strategic Priority Research Program of Chinese Academy of Sciences ; strategic Priority Research Program of Chinese Academy of Sciences ; Open Fund of the State Key Laboratory of Astronautic Dynamics of China ; Open Fund of the State Key Laboratory of Astronautic Dynamics of China ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Young Researcher Grant of National Astronomical Observatories Chinese Academy of Sciences ; Young Researcher Grant of National Astronomical Observatories Chinese Academy of Sciences ; Key Research Program of the Chinese Academy of Sciences ; Key Research Program of the Chinese Academy of Sciences ; strategic Priority Research Program of Chinese Academy of Sciences ; strategic Priority Research Program of Chinese Academy of Sciences ; Open Fund of the State Key Laboratory of Astronautic Dynamics of China ; Open Fund of the State Key Laboratory of Astronautic Dynamics of China ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Young Researcher Grant of National Astronomical Observatories Chinese Academy of Sciences ; Young Researcher Grant of National Astronomical Observatories Chinese Academy of Sciences ; Key Research Program of the Chinese Academy of Sciences ; Key Research Program of the Chinese Academy of Sciences ; strategic Priority Research Program of Chinese Academy of Sciences ; strategic Priority Research Program of Chinese Academy of Sciences ; Open Fund of the State Key Laboratory of Astronautic Dynamics of China ; Open Fund of the State Key Laboratory of Astronautic Dynamics of China ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences ; Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences
内容类型	期刊论文
源URL	[http://ir.bao.ac.cn/handle/114a11/23131]
专题	中国科学院国家天文台
通讯作者	Wang, P. F.
作者单位	1.State Key Lab Astronaut Dynam, Xian 710043, Shaanxi, Peoples R China 2.Chinese Acad Sci, Natl Astron Observ, Jia 20 Datun Rd, Beijing 100101, Peoples R China 3.China Xian Satellite Control Ctr, Jiamusi Deep Space Stn, Jiamusi 154002, Heilongjiang, Peoples R China 4.Univ Chinese Acad Sci, Sch Astron, Beijing 100049, Peoples R China 5.Chinese Acad Sci, CAS Key Lab FAST, NAOC, Beijing 100101, Peoples R China
推荐引用方式 GB/T 7714	Wang, P. F.,Han, J. L.,Han, L.,et al. Jiamusi pulsar observations II. Scintillations of ten pulsars[J]. ASTRONOMY & ASTROPHYSICS,2018,618:15.
APA	Wang, P. F..,Han, J. L..,Han, L..,Zhang, J. H..,Li, J. Q..,...&Gao, X. Y..(2018).Jiamusi pulsar observations II. Scintillations of ten pulsars.ASTRONOMY & ASTROPHYSICS,618,15.
MLA	Wang, P. F.,et al."Jiamusi pulsar observations II. Scintillations of ten pulsars".ASTRONOMY & ASTROPHYSICS 618(2018):15.