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Precision Orbital Dynamics from Interstellar Scintillation Arcs for PSR J0437–4715
Reardon,Daniel J.1,2; Coles,William A.3; Bailes,Matthew1,2; Bhat,N. D. Ramesh4; Dai,Shi5; Hobbs,George B.2,5; Kerr,Matthew6; Manchester,Richard N.5; Os?owski,Stefan1; Parthasarathy,Aditya1,2; Russell,Christopher J.7; Shannon,Ryan M.1,2; Spiewak,Renée1,2; Toomey,Lawrence5; Tuntsov,Artem V.8; van Straten,Willem9; Walker,Mark A.8; Wang,Jingbo10; Zhang,Lei5,11,12; Zhu,Xing-Jiang2,13
2020-11-25
Source PublicationThe Astrophysical Journal
ISSN0004-637X
Volume904Issue:2
AbstractAbstract Intensity scintillations of radio pulsars are known to originate from interference between waves scattered by the electron density irregularities of interstellar plasma, often leading to parabolic arcs in the two-dimensional power spectrum of the recorded dynamic spectrum. The degree of arc curvature depends on the distance to the scattering plasma and its transverse velocity with respect to the line of sight. We report the observation of annual and orbital variations in the curvature of scintillation arcs over a period of 16 yr for the bright millisecond pulsar, PSR?J0437?4715. These variations are the signature of the relative transverse motions of Earth, the pulsar, and the scattering medium, which we model to obtain precise measurements of parameters of the pulsar’s binary orbit and the scattering medium itself. We observe two clear scintillation arcs in most of our >5000 observations, and we show that they originate from scattering by thin screens located at distances D1?=?89.8?±?0.4 pc and D2?=?124?±?3 pc from Earth. The best-fit scattering model we derive for the brightest arc yields the pulsar’s orbital inclination angle, i?=?137.°1?±?0.°3, and longitude of ascending node, Ω?=?206.°3?±?0.°4. Using scintillation arcs for precise astrometry and orbital dynamics can be superior to modeling variations in the diffractive scintillation timescale, because the arc curvature is independent of variations in the level of turbulence of interstellar plasma. This technique can be used in combination with pulsar timing to determine the full three-dimensional orbital geometries of binary pulsars and provides parameters essential for testing theories of gravity and constraining neutron star masses.
KeywordPulsars Millisecond pulsars Interstellar medium Interstellar plasma Binary pulsars Radio pulsars Interstellar scintillation Radio astronomy Orbital motion Astrometry Orbits Orbit determination
DOI10.3847/1538-4357/abbd40
Language英语
WOS IDIOP:0004-637X-904-2-abbd40
PublisherThe American Astronomical Society
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/62430
Collection中国科学院国家天文台
Corresponding AuthorReardon,Daniel J.
Affiliation1.Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC 3122, Australia; dreardon@swin.edu.au
2.Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), Australia
3.Electrical and Computer Engineering, University of California at San Diego, La Jolla, CA, USA
4.International Centre for Radio Astronomy Research, Curtin University, Bentley, WA 6102, Australia
5.Australia Telescope National Facility, CSIRO Astronomy & Space Science, P.O. Box 76, Epping, NSW 1710, Australia
6.Space Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USA
7.CSIRO Scientific Computing Services, Australian Technology Park, Locked Bag 9013, Alexandria, NSW 1435, Australia
8.Manly Astrophysics, 15/41-42 East Esplanade, Manly, NSW 2095, Australia
9.Institute for Radio Astronomy & Space Research, Auckland University of Technology, Private Bag 92006, Auckland 1142, New Zealand
10.Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of China
11.National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China
12.University of the Chinese Academy of Sciences, Beijing 100049, People’s Republic of China
13.School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia
Recommended Citation
GB/T 7714
Reardon,Daniel J.,Coles,William A.,Bailes,Matthew,等. Precision Orbital Dynamics from Interstellar Scintillation Arcs for PSR J0437–4715[J]. The Astrophysical Journal,2020,904(2).
APA Reardon,Daniel J..,Coles,William A..,Bailes,Matthew.,Bhat,N. D. Ramesh.,Dai,Shi.,...&Zhu,Xing-Jiang.(2020).Precision Orbital Dynamics from Interstellar Scintillation Arcs for PSR J0437–4715.The Astrophysical Journal,904(2).
MLA Reardon,Daniel J.,et al."Precision Orbital Dynamics from Interstellar Scintillation Arcs for PSR J0437–4715".The Astrophysical Journal 904.2(2020).
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