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Radio Pulse Properties of the Millisecond Pulsar PSR J0437-4715

Jenet, F. A. and Anderson, S. B. and Kaspi, V. M. and Prince, Thomas A. and Unwin, S. C. (1998) Radio Pulse Properties of the Millisecond Pulsar PSR J0437-4715. Astrophysical Journal, 498 (1). pp. 365-372. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20150107-163008655

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Abstract

We present a total of 48 minutes of observations of the nearby, bright millisecond pulsar PSR J0437[4715 taken at the Parkes Observatory in Australia. The data were obtained at a central radio frequency of 1380 MHz using a high-speed tape recorder that permitted coherent Nyquist sampling of 50 MHz of bandwidth in each of two polarizations. Using the high time resolution available from this voltage recording technique, we have studied a variety of single-pulse properties, many for the first time in a millisecond pulsar. We show that individual pulses are broad band, have pulse widths ranging from ~10 (~0°.6 in pulse longitude) to ~300 us (~20°) with a mean pulse width of ~65 us (~4°), exhibit a wide variety of morphologies, and can be highly linearly polarized. Single pulse peaks can be as high as 205 Jy (over ~40 times the average pulse peak), and have a probability distribution similar to those of slow-rotating pulsars. We observed no single pulse energy exceeding ~4.4 times the average pulse energy, ruling out "giant pulses" as have been seen for the Crab and PSR B1937+21 pulsars. PSR J0437[4715 does not exhibit classical microstructure or show any signs of a preferred timescale that could be associated with primary emitters ; single pulse modulation has been observed to be consistent with amplitude-modulated noise down to timescales of 80 ns. We observe a significant inverse correlation between pulse peak and width. Thus, the average pulse proÐle produced by selecting for large pulse peaks is narrower than the standard average profile. We find no evidence for "diffractive" quantization e†ects in the individual pulse arrival times or amplitudes as have been reported for this pulsar at lower radio frequency using coarser time resolution. Overall, we find that the single-pulse properties of PSR J0437-4715 are similar to those of the common slow-rotating pulsars, even though this pulsar's magnetosphere and surface magnetic field are several orders of magnitude smaller than those of the general population. The pulsar radio emission mechanism must therefore be insensitive to these fundamental neutron star properties.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1086/305529DOIArticle
ORCID:
AuthorORCID
Kaspi, V. M.0000-0001-9345-0307
Prince, Thomas A.0000-0002-8850-3627
Additional Information:© 1998. The American Astronomical Society. Received 1997 July 8; accepted 1997 December 12. We thank Jagmit Sandhu, Shri Kulkarni, and Don Backer for helpful conversations. We thank Matthew Bailes and Jagmit Sandhu for sharing observing time. This research was supported in part by the National Science Foundation grant ASC 93-18145. V. M. K. received support from Hubble Fellowship grant HF-1061.01-94A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NSFASC 93-18145
NASA Hubble FellowshipHF-106101-94A
NASANAS 5-26555
Non-Subject Keywords:pulsars: individual (J0437-4715); radio continuum: stars: neutron
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory1998-12
Issue or Number:1
Record Number:CaltechAUTHORS:20150107-163008655
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20150107-163008655
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:53303
Collection:CaltechAUTHORS
Deposited By: Deborah Miles
Deposited On:09 Jan 2015 17:10
Last Modified:04 Dec 2019 20:17

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