skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: CORRELATION OF CHANDRA PHOTONS WITH THE RADIO GIANT PULSES FROM THE CRAB PULSAR

Abstract

No apparent correlation was found between giant pulses (GPs) and X-ray photons from the Crab pulsar during 5.4 hr of simultaneous observations with the Green Bank Telescope at 1.5 GHz and Chandra X-Ray Observatory primarily in the energy range of 1.5-4.5 keV. During the Crab pulsar periods with GPs, the X-ray flux in radio emission phase windows does not change more than by {+-}10% for main pulse (MP) GPs and {+-}30% for interpulse (IP) GPs. During GPs themselves, the X-ray flux does not change by more than two times for MP GPs and five times for IP GPs. All limits quoted are compatible with 2{sigma} fluctuations of the X-ray flux around the sets of false GPs with random arrival times. The results speak in favor of changes in plasma coherence as the origin of GPs. However, the results do not rule out variations in the rate of particle creation if the particles that emit coherent radio emission are mostly at the lowest Landau level.

Authors:
 [1];  [2];  [3]
  1. Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904 (United States)
  2. Department of Physics, West Virginia University, Morgantown, WV 26506 (United States)
  3. Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo (Netherlands)
Publication Date:
OSTI Identifier:
22020514
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 749; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; PHOTONS; PULSARS; RANDOMNESS; STARS; TELESCOPES

Citation Formats

Bilous, A V, McLaughlin, M A, Kondratiev, V I, and Ransom, S. M., E-mail: avb3k@virginia.edu. CORRELATION OF CHANDRA PHOTONS WITH THE RADIO GIANT PULSES FROM THE CRAB PULSAR. United States: N. p., 2012. Web. doi:10.1088/0004-637X/749/1/24.
Bilous, A V, McLaughlin, M A, Kondratiev, V I, & Ransom, S. M., E-mail: avb3k@virginia.edu. CORRELATION OF CHANDRA PHOTONS WITH THE RADIO GIANT PULSES FROM THE CRAB PULSAR. United States. https://doi.org/10.1088/0004-637X/749/1/24
Bilous, A V, McLaughlin, M A, Kondratiev, V I, and Ransom, S. M., E-mail: avb3k@virginia.edu. 2012. "CORRELATION OF CHANDRA PHOTONS WITH THE RADIO GIANT PULSES FROM THE CRAB PULSAR". United States. https://doi.org/10.1088/0004-637X/749/1/24.
@article{osti_22020514,
title = {CORRELATION OF CHANDRA PHOTONS WITH THE RADIO GIANT PULSES FROM THE CRAB PULSAR},
author = {Bilous, A V and McLaughlin, M A and Kondratiev, V I and Ransom, S. M., E-mail: avb3k@virginia.edu},
abstractNote = {No apparent correlation was found between giant pulses (GPs) and X-ray photons from the Crab pulsar during 5.4 hr of simultaneous observations with the Green Bank Telescope at 1.5 GHz and Chandra X-Ray Observatory primarily in the energy range of 1.5-4.5 keV. During the Crab pulsar periods with GPs, the X-ray flux in radio emission phase windows does not change more than by {+-}10% for main pulse (MP) GPs and {+-}30% for interpulse (IP) GPs. During GPs themselves, the X-ray flux does not change by more than two times for MP GPs and five times for IP GPs. All limits quoted are compatible with 2{sigma} fluctuations of the X-ray flux around the sets of false GPs with random arrival times. The results speak in favor of changes in plasma coherence as the origin of GPs. However, the results do not rule out variations in the rate of particle creation if the particles that emit coherent radio emission are mostly at the lowest Landau level.},
doi = {10.1088/0004-637X/749/1/24},
url = {https://www.osti.gov/biblio/22020514}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 1,
volume = 749,
place = {United States},
year = {Tue Apr 10 00:00:00 EDT 2012},
month = {Tue Apr 10 00:00:00 EDT 2012}
}