| Title | A revisit of PSR J1909-3744 with 15-yr high-precision timing |
| Authors | Liu, K. Guillemot, L. Istrate, A. G. Shao, L. Tauris, T. M. Wex, N. Antoniadis, J. Chalumeau, A. Cognard, I Desvignes, G. Freire, P. C. C. Kehl, M. S. Theureau, G. |
| Affiliation | Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany CNRS INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France Univ Orleans CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China Aarhus Univ, Aarhus Inst Adv Studies AIAS, Hoegh Guldbergs Gade 6B, DK-8000 Aarhus C, Denmark Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark AIFA Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany Univ Crete, Inst Astrophys, Dept Phys, FORTH, Univ Campus, GR-71003 Iraklion, Greece Univ Paris, Sorbonne Univ, CNRS, LESIA,Observ Paris,Univ PSL, 5 Pl Jules Janssen, F-92195 Meudon, France Univ Paris, Ctr Natl Rech Sci, Univ Paris Sci & Lettres, Lab Univers & Theories,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France |
| Keywords | WHITE-DWARF COMPANIONS MILLISECOND PULSARS RELATIVISTIC GRAVITY SCALAR THEORIES ORBITAL PERIOD SOLAR-SYSTEM BINARY MASS EVOLUTION TESTS |
| Issue Date | Dec-2020 |
| Publisher | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY |
| Abstract | We report on a high-precision timing analysis and an astrophysical study of the binary millisecond pulsar, PSR J1909-3744, motivated by the accumulation of data with well improved quality over the past decade. Using 15 yr of observations with the Nancay Radio Telescope, we achieve a timing precision of approximately 100 ns. We verify our timing results by using both broad-band and sub-band template matching methods to create the pulse time-of-arrivals. Compared with previous studies, we improve the measurement precision of secular changes in orbital period and projected semimajor axis. We show that these variations are both dominated by the relative motion between the pulsar system and the Solar system barycentre. Additionally, we identified four possible solutions to the ascending node of the pulsar orbit, and measured a precise kinetic distance of the system. Using our timing measurements and published optical observations, we investigate the binary history of this system using the stellar evolution code MESA, and discuss solutions based on detailed WD cooling at the edge of the WD age dichotomy paradigm. We determine the 3D velocity of the system and show that it has been undergoing a highly eccentric orbit around the centre of our Galaxy. Furthermore, we set up a constraint over dipolar gravitational radiation with the system, which is complementary to previous studies given the mass of the pulsar. We also obtain a new limit on the parametrized post-Newtonian parameter, vertical bar(alpha) over cap (1)vertical bar < 2.1 x 10(-5) at 95 per cent confidence level, which is fractionally better than previous best published value and achieved with a more concrete method. |
| URI | http://hdl.handle.net/20.500.11897/599354 |
| ISSN | 0035-8711 |
| DOI | 10.1093/mnras/staa2993 |
| Indexed | SCI(E) |
| Appears in Collections: | 科维理天文与天体物理研究所 |
