The Astrophysical Journal (Jan 2024)
RRAT J1913+1330: An Extremely Variable and Puzzling Pulsar
- S. B. Zhang,
- J. J. Geng,
- J. S. Wang,
- X. Yang,
- J. Kaczmarek,
- Z. F. Tang,
- S. Johnston,
- G. Hobbs,
- R. Manchester,
- X. F. Wu,
- P. Jiang,
- Y. F. Huang,
- Y. C. Zou,
- Z. G. Dai,
- B. Zhang,
- D. Li,
- Y. P. Yang,
- S. Dai,
- C. M. Chang,
- Z. C. Pan,
- J. G. Lu,
- J. J. Wei,
- Y. Li,
- Q. W. Wu,
- L. Qian,
- P. Wang,
- S. Q. Wang,
- Y. Feng,
- L. Staveley-Smith
Affiliations
- S. B. Zhang
- ORCiD
- Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People's Republic of China ; [email protected]
- J. J. Geng
- Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People's Republic of China ; [email protected]
- J. S. Wang
- ORCiD
- Max-Planck-Institut für Kernphysik , Saupfercheckweg 1, D-69117 Heidelberg, Germany
- X. Yang
- ORCiD
- Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People's Republic of China ; [email protected]; School of Astronomy and Space Sciences, University of Science and Technology of China , Hefei 230026, People's Republic of China
- J. Kaczmarek
- CSIRO Space and Astronomy , Epping, NSW 1710, Australia; Department of Computer Science, Math, Physics, & Statistics, University of British Columbia , Kelowna, BC V1V 1V7, Canada
- Z. F. Tang
- Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People's Republic of China ; [email protected]; School of Astronomy and Space Sciences, University of Science and Technology of China , Hefei 230026, People's Republic of China
- S. Johnston
- CSIRO Space and Astronomy , Epping, NSW 1710, Australia
- G. Hobbs
- CSIRO Space and Astronomy , Epping, NSW 1710, Australia
- R. Manchester
- CSIRO Space and Astronomy , Epping, NSW 1710, Australia
- X. F. Wu
- Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People's Republic of China ; [email protected]; School of Astronomy and Space Sciences, University of Science and Technology of China , Hefei 230026, People's Republic of China
- P. Jiang
- ORCiD
- National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; [email protected]; CAS Key laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China
- Y. F. Huang
- School of Astronomy and Space Science, Nanjing University , Nanjing 210023, People's Republic of China
- Y. C. Zou
- School of Physics, Huazhong University of Science and Technology , Wuhan 430074, People's Republic of China
- Z. G. Dai
- Department of Astronomy, University of Science and Technology of China , Hefei 230026, People's Republic of China ; [email protected]
- B. Zhang
- ORCiD
- Department of Physics and Astronomy, University of Nevada , Las Vegas, NV 89154, USA ; [email protected]
- D. Li
- ORCiD
- National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; [email protected]; Research Center for Intelligent Computing Platforms , Zhejiang Laboratory, Hangzhou 311100, People's Republic of China; University of Chinese Academy of Sciences , Beijing 100049, People's Republic of China
- Y. P. Yang
- Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People's Republic of China ; [email protected]; South-Western Institute for Astronomy Research, Yunnan University , Kunming 650504, People's Republic of China
- S. Dai
- School of Science, Western Sydney University , Locked Bag 1797, Penrith NSW 2751, Australia
- C. M. Chang
- Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People's Republic of China ; [email protected]; School of Astronomy and Space Sciences, University of Science and Technology of China , Hefei 230026, People's Republic of China
- Z. C. Pan
- National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; [email protected]; CAS Key laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China
- J. G. Lu
- National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; [email protected]; CAS Key laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China
- J. J. Wei
- Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People's Republic of China ; [email protected]
- Y. Li
- Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People's Republic of China ; [email protected]
- Q. W. Wu
- School of Physics, Huazhong University of Science and Technology , Wuhan 430074, People's Republic of China
- L. Qian
- ORCiD
- National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; [email protected]; CAS Key laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China
- P. Wang
- National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of China ; [email protected]; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People's Republic of China
- S. Q. Wang
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences , Science 1-Street, Urumqi, Xinjiang 830011, People's Republic of China
- Y. Feng
- Research Center for Intelligent Computing Platforms , Zhejiang Laboratory, Hangzhou 311100, People's Republic of China
- L. Staveley-Smith
- International Centre for Radio Astronomy Research, University of Western Australia , Crawley, WA 6009, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , Australia
- DOI
- https://doi.org/10.3847/1538-4357/ad6602
- Journal volume & issue
-
Vol. 972,
no. 1
p. 59
Abstract
Rotating radio transients (RRATs) are neutron stars that emit sporadic radio bursts. We detected 1955 single pulses from RRAT J1913+1330 using the 19 beam receiver of the Five-hundred-meter Aperture Spherical radio Telescope. These pulses were detected in 19 distinct clusters, with 49.4% of them occurring with a waiting time of one rotation period. The energy distribution of these individual pulses exhibited a wide range, spanning 3 orders of magnitude, reminiscent of repeating fast radio bursts (FRBs). Furthermore, we observed abrupt variations in pulse profile, width, peak flux, and fluence between adjacent sequential pulses. These findings suggest that this RRAT could be interpreted as a pulsar with extreme pulse-to-pulse modulation. The presence of sequential pulse trains during active phases, along with significant pulse variations in profile, fluence, flux, and width, should be intrinsic to a subset of RRATs. Our results indicate that J1913+1330 represents a peculiar source that shares certain properties with populations of nulling pulsars, giant pulses, and FRBs from different perspectives. The dramatic pulse-to-pulse variation observed in J1913+1330 could be attributed to unstable pair creation above the polar cap region and the variation of the site where streaming pairs emit coherently. Exploring a larger sample of RRATs exhibiting similar properties to J1913+1330 has the potential to significantly advance our understanding of pulsars, RRATs, and FRBs.
Keywords
