Simultaneous single-pulse observations of radio pulsars V. On the broadband nature of the pulse nulling phenomenon in PSR B1133+16
Identifieur interne : 003E41 ( PascalFrancis/Corpus ); précédent : 003E40; suivant : 003E42Simultaneous single-pulse observations of radio pulsars V. On the broadband nature of the pulse nulling phenomenon in PSR B1133+16
Auteurs : N. D. R. Bhat ; Y. Gupta ; M. Kramer ; A. Karastergiou ; A. G. Lyne ; S. JohnstonSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2007.
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Abstract
Aims. In this paper we revisit the well-known phenomenon of pulse nulling using high-quality single-pulse data of PSR B 1133+16 from simultaneous multifrequency observations. Methods. Observations were made at 325, 610, 1400 and 4850 MHz as part of a joint program between the European Pulsar Network (EPN) and the Giant Metrewave Radio Telescope (GMRT). The pulse energy time series are analysed to derive improved statistics of nulling pulses as well as to investigate the frequency dependence of the phenomenon. Results. The pulsar is observed to be in null state for approximately 15% of the time; however, we find that nulling does not always occur simultaneously at all four frequencies of observation. We characterise the statistics of such "selective nulling" as a function of frequency, separation in frequency, and combination of frequencies. The most remarkable case of such selective nulling seen in our data is a significantly large number of nulls (≃6%) at lower frequencies, that are marked by the presence of a fairly narrow emission feature at the highest frequency of 4850 MHz. We refer to these as "low frequency (LF) nulls". We characterise the properties of high frequency (HF) emission at the occurrence of LF nulls, and compare and contrast them with that of "normal emission" at 4850 MHz. Our analysis shows that this high frequency emission tends to occur preferentially over a narrow range in longitude and with pulse widths typically of the order of a few milliseconds. We discuss the implications of our results for the pulsar emission mechanism in general and for the broadbandness of nulling phenomenon in particular. Our results signify the presence of an additional process of emission which does not turn off when the pulsar nulls at low frequencies, and becomes more prominent at higher frequencies. Our analysis also hints at a possible outer gap origin for this new population of pulses, and thus a likely connection to some high-energy emission processes that occur in the outer parts of the pulsar magnetosphere.
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| NO : | PASCAL 07-0061207 INIST |
|---|---|
| ET : | Simultaneous single-pulse observations of radio pulsars V. On the broadband nature of the pulse nulling phenomenon in PSR B1133+16 |
| AU : | BHAT (N. D. R.); GUPTA (Y.); KRAMER (M.); KARASTERGIOU (A.); LYNE (A. G.); JOHNSTON (S.) |
| AF : | Centre for Astrophysics and Supercomputing, Swinburne University of Technology/Hawthorn, Vic 3122/Australie (1 aut.); National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Ganeshkhind/Pune 411007/Inde (2 aut.); Jodrell Bank Observatory, University of Manchester/Macclesfield, Cheshire, SKI 1 9DL/Royaume-Uni (3 aut., 5 aut.); IRAM, 300 rue de la Piscine, Domaine Universitaire/38406 Saint Martin d'H========Atilde;ires/France (4 aut.); Australia Telescope National Facility, CSIRO, PO Box 76/Epping, NSW 1710/Australie (6 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2007; Vol. 462; No. 1; Pp. 257-268; Bibl. 30 ref. |
| LA : | Anglais |
| EA : | Aims. In this paper we revisit the well-known phenomenon of pulse nulling using high-quality single-pulse data of PSR B 1133+16 from simultaneous multifrequency observations. Methods. Observations were made at 325, 610, 1400 and 4850 MHz as part of a joint program between the European Pulsar Network (EPN) and the Giant Metrewave Radio Telescope (GMRT). The pulse energy time series are analysed to derive improved statistics of nulling pulses as well as to investigate the frequency dependence of the phenomenon. Results. The pulsar is observed to be in null state for approximately 15% of the time; however, we find that nulling does not always occur simultaneously at all four frequencies of observation. We characterise the statistics of such "selective nulling" as a function of frequency, separation in frequency, and combination of frequencies. The most remarkable case of such selective nulling seen in our data is a significantly large number of nulls (≃6%) at lower frequencies, that are marked by the presence of a fairly narrow emission feature at the highest frequency of 4850 MHz. We refer to these as "low frequency (LF) nulls". We characterise the properties of high frequency (HF) emission at the occurrence of LF nulls, and compare and contrast them with that of "normal emission" at 4850 MHz. Our analysis shows that this high frequency emission tends to occur preferentially over a narrow range in longitude and with pulse widths typically of the order of a few milliseconds. We discuss the implications of our results for the pulsar emission mechanism in general and for the broadbandness of nulling phenomenon in particular. Our results signify the presence of an additional process of emission which does not turn off when the pulsar nulls at low frequencies, and becomes more prominent at higher frequencies. Our analysis also hints at a possible outer gap origin for this new population of pulses, and thus a likely connection to some high-energy emission processes that occur in the outer parts of the pulsar magnetosphere. |
| CC : | 001E03 |
| FD : | Observation simultanée; Observation radio; Pulsar radio; Observation multifréquence; Série temporelle; Dépendance fréquence; Magnétosphère stellaire; Rayonnement non thermique |
| ED : | Simultaneous observation; Radio observation; Radiopulsar; Multifrequency observation; Time series; Frequency dependence; Stellar magnetospheres; Nonthermal radiation |
| SD : | Observación simultánea; Observación radio; Pulsar radio; Observación multifrecuencia |
| LO : | INIST-14176.354000159602800300 |
| ID : | 07-0061207 |
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Kramer</name><affiliation><inist:fA14 i1="03"><s1>Jodrell Bank Observatory, University of Manchester</s1><s2>Macclesfield, Cheshire, SKI 1 9DL</s2><s3>GBR</s3><sZ>3 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Karastergiou, A" sort="Karastergiou, A" uniqKey="Karastergiou A" first="A." last="Karastergiou">A. Karastergiou</name><affiliation><inist:fA14 i1="04"><s1>IRAM, 300 rue de la Piscine, Domaine Universitaire</s1><s2>38406 Saint Martin d'H========Atilde;ires</s2><s3>FRA</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lyne, A G" sort="Lyne, A G" uniqKey="Lyne A" first="A. G." last="Lyne">A. G. Lyne</name><affiliation><inist:fA14 i1="03"><s1>Jodrell Bank Observatory, University of Manchester</s1><s2>Macclesfield, Cheshire, SKI 1 9DL</s2><s3>GBR</s3><sZ>3 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Johnston, S" sort="Johnston, S" uniqKey="Johnston S" first="S." last="Johnston">S. Johnston</name><affiliation><inist:fA14 i1="05"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">07-0061207</idno><date when="2007">2007</date><idno type="stanalyst">PASCAL 07-0061207 INIST</idno><idno type="RBID">Pascal:07-0061207</idno><idno type="wicri:Area/PascalFrancis/Corpus">003E41</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Simultaneous single-pulse observations of radio pulsars V. On the broadband nature of the pulse nulling phenomenon in PSR B1133+16</title><author><name sortKey="Bhat, N D R" sort="Bhat, N D R" uniqKey="Bhat N" first="N. D. R." last="Bhat">N. D. R. Bhat</name><affiliation><inist:fA14 i1="01"><s1>Centre for Astrophysics and Supercomputing, Swinburne University of Technology</s1><s2>Hawthorn, Vic 3122</s2><s3>AUS</s3><sZ>1 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gupta, Y" sort="Gupta, Y" uniqKey="Gupta Y" first="Y." last="Gupta">Y. Gupta</name><affiliation><inist:fA14 i1="02"><s1>National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Ganeshkhind</s1><s2>Pune 411007</s2><s3>IND</s3><sZ>2 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kramer, M" sort="Kramer, M" uniqKey="Kramer M" first="M." last="Kramer">M. Kramer</name><affiliation><inist:fA14 i1="03"><s1>Jodrell Bank Observatory, University of Manchester</s1><s2>Macclesfield, Cheshire, SKI 1 9DL</s2><s3>GBR</s3><sZ>3 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Karastergiou, A" sort="Karastergiou, A" uniqKey="Karastergiou A" first="A." last="Karastergiou">A. Karastergiou</name><affiliation><inist:fA14 i1="04"><s1>IRAM, 300 rue de la Piscine, Domaine Universitaire</s1><s2>38406 Saint Martin d'H========Atilde;ires</s2><s3>FRA</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lyne, A G" sort="Lyne, A G" uniqKey="Lyne A" first="A. G." last="Lyne">A. G. Lyne</name><affiliation><inist:fA14 i1="03"><s1>Jodrell Bank Observatory, University of Manchester</s1><s2>Macclesfield, Cheshire, SKI 1 9DL</s2><s3>GBR</s3><sZ>3 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Johnston, S" sort="Johnston, S" uniqKey="Johnston S" first="S." last="Johnston">S. Johnston</name><affiliation><inist:fA14 i1="05"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2007">2007</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Frequency dependence</term><term>Multifrequency observation</term><term>Nonthermal radiation</term><term>Radio observation</term><term>Radiopulsar</term><term>Simultaneous observation</term><term>Stellar magnetospheres</term><term>Time series</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Observation simultanée</term><term>Observation radio</term><term>Pulsar radio</term><term>Observation multifréquence</term><term>Série temporelle</term><term>Dépendance fréquence</term><term>Magnétosphère stellaire</term><term>Rayonnement non thermique</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Aims. In this paper we revisit the well-known phenomenon of pulse nulling using high-quality single-pulse data of PSR B 1133+16 from simultaneous multifrequency observations. Methods. Observations were made at 325, 610, 1400 and 4850 MHz as part of a joint program between the European Pulsar Network (EPN) and the Giant Metrewave Radio Telescope (GMRT). The pulse energy time series are analysed to derive improved statistics of nulling pulses as well as to investigate the frequency dependence of the phenomenon. Results. The pulsar is observed to be in null state for approximately 15% of the time; however, we find that nulling does not always occur simultaneously at all four frequencies of observation. We characterise the statistics of such "selective nulling" as a function of frequency, separation in frequency, and combination of frequencies. The most remarkable case of such selective nulling seen in our data is a significantly large number of nulls (≃6%) at lower frequencies, that are marked by the presence of a fairly narrow emission feature at the highest frequency of 4850 MHz. We refer to these as "low frequency (LF) nulls". We characterise the properties of high frequency (HF) emission at the occurrence of LF nulls, and compare and contrast them with that of "normal emission" at 4850 MHz. Our analysis shows that this high frequency emission tends to occur preferentially over a narrow range in longitude and with pulse widths typically of the order of a few milliseconds. We discuss the implications of our results for the pulsar emission mechanism in general and for the broadbandness of nulling phenomenon in particular. Our results signify the presence of an additional process of emission which does not turn off when the pulsar nulls at low frequencies, and becomes more prominent at higher frequencies. Our analysis also hints at a possible outer gap origin for this new population of pulses, and thus a likely connection to some high-energy emission processes that occur in the outer parts of the pulsar magnetosphere.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-6361</s0></fA01><fA02 i1="01"><s0>AAEJAF</s0></fA02><fA03 i2="1"><s0>Astron. astrophys. : (Berl., Print)</s0></fA03><fA05><s2>462</s2></fA05><fA06><s2>1</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Simultaneous single-pulse observations of radio pulsars V. On the broadband nature of the pulse nulling phenomenon in PSR B1133+16</s1></fA08><fA11 i1="01" i2="1"><s1>BHAT (N. D. R.)</s1></fA11><fA11 i1="02" i2="1"><s1>GUPTA (Y.)</s1></fA11><fA11 i1="03" i2="1"><s1>KRAMER (M.)</s1></fA11><fA11 i1="04" i2="1"><s1>KARASTERGIOU (A.)</s1></fA11><fA11 i1="05" i2="1"><s1>LYNE (A. G.)</s1></fA11><fA11 i1="06" i2="1"><s1>JOHNSTON (S.)</s1></fA11><fA14 i1="01"><s1>Centre for Astrophysics and Supercomputing, Swinburne University of Technology</s1><s2>Hawthorn, Vic 3122</s2><s3>AUS</s3><sZ>1 aut.</sZ></fA14><fA14 i1="02"><s1>National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Ganeshkhind</s1><s2>Pune 411007</s2><s3>IND</s3><sZ>2 aut.</sZ></fA14><fA14 i1="03"><s1>Jodrell Bank Observatory, University of Manchester</s1><s2>Macclesfield, Cheshire, SKI 1 9DL</s2><s3>GBR</s3><sZ>3 aut.</sZ><sZ>5 aut.</sZ></fA14><fA14 i1="04"><s1>IRAM, 300 rue de la Piscine, Domaine Universitaire</s1><s2>38406 Saint Martin d'H========Atilde;ires</s2><s3>FRA</s3><sZ>4 aut.</sZ></fA14><fA14 i1="05"><s1>Australia Telescope National Facility, CSIRO, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>6 aut.</sZ></fA14><fA20><s1>257-268</s1></fA20><fA21><s1>2007</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000159602800300</s5></fA43><fA44><s0>0000</s0><s1>© 2007 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>30 ref.</s0></fA45><fA47 i1="01" i2="1"><s0>07-0061207</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0></fA64><fA66 i1="01"><s0>FRA</s0></fA66><fC01 i1="01" l="ENG"><s0>Aims. In this paper we revisit the well-known phenomenon of pulse nulling using high-quality single-pulse data of PSR B 1133+16 from simultaneous multifrequency observations. Methods. Observations were made at 325, 610, 1400 and 4850 MHz as part of a joint program between the European Pulsar Network (EPN) and the Giant Metrewave Radio Telescope (GMRT). The pulse energy time series are analysed to derive improved statistics of nulling pulses as well as to investigate the frequency dependence of the phenomenon. Results. The pulsar is observed to be in null state for approximately 15% of the time; however, we find that nulling does not always occur simultaneously at all four frequencies of observation. We characterise the statistics of such "selective nulling" as a function of frequency, separation in frequency, and combination of frequencies. The most remarkable case of such selective nulling seen in our data is a significantly large number of nulls (≃6%) at lower frequencies, that are marked by the presence of a fairly narrow emission feature at the highest frequency of 4850 MHz. We refer to these as "low frequency (LF) nulls". We characterise the properties of high frequency (HF) emission at the occurrence of LF nulls, and compare and contrast them with that of "normal emission" at 4850 MHz. Our analysis shows that this high frequency emission tends to occur preferentially over a narrow range in longitude and with pulse widths typically of the order of a few milliseconds. We discuss the implications of our results for the pulsar emission mechanism in general and for the broadbandness of nulling phenomenon in particular. Our results signify the presence of an additional process of emission which does not turn off when the pulsar nulls at low frequencies, and becomes more prominent at higher frequencies. Our analysis also hints at a possible outer gap origin for this new population of pulses, and thus a likely connection to some high-energy emission processes that occur in the outer parts of the pulsar magnetosphere.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Observation simultanée</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Simultaneous observation</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Observación simultánea</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Observation radio</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Radio observation</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Observación radio</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Pulsar radio</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Radiopulsar</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Pulsar radio</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Observation multifréquence</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Multifrequency observation</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Observación multifrecuencia</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Série temporelle</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Time series</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Dépendance fréquence</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Frequency dependence</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Magnétosphère stellaire</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Stellar magnetospheres</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Rayonnement non thermique</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Nonthermal radiation</s0><s5>33</s5></fC03><fN21><s1>036</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 07-0061207 INIST</NO><ET>Simultaneous single-pulse observations of radio pulsars V. On the broadband nature of the pulse nulling phenomenon in PSR B1133+16</ET><AU>BHAT (N. D. R.); GUPTA (Y.); KRAMER (M.); KARASTERGIOU (A.); LYNE (A. G.); JOHNSTON (S.)</AU><AF>Centre for Astrophysics and Supercomputing, Swinburne University of Technology/Hawthorn, Vic 3122/Australie (1 aut.); National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Ganeshkhind/Pune 411007/Inde (2 aut.); Jodrell Bank Observatory, University of Manchester/Macclesfield, Cheshire, SKI 1 9DL/Royaume-Uni (3 aut., 5 aut.); IRAM, 300 rue de la Piscine, Domaine Universitaire/38406 Saint Martin d'H========Atilde;ires/France (4 aut.); Australia Telescope National Facility, CSIRO, PO Box 76/Epping, NSW 1710/Australie (6 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2007; Vol. 462; No. 1; Pp. 257-268; Bibl. 30 ref.</SO><LA>Anglais</LA><EA>Aims. In this paper we revisit the well-known phenomenon of pulse nulling using high-quality single-pulse data of PSR B 1133+16 from simultaneous multifrequency observations. Methods. Observations were made at 325, 610, 1400 and 4850 MHz as part of a joint program between the European Pulsar Network (EPN) and the Giant Metrewave Radio Telescope (GMRT). The pulse energy time series are analysed to derive improved statistics of nulling pulses as well as to investigate the frequency dependence of the phenomenon. Results. The pulsar is observed to be in null state for approximately 15% of the time; however, we find that nulling does not always occur simultaneously at all four frequencies of observation. We characterise the statistics of such "selective nulling" as a function of frequency, separation in frequency, and combination of frequencies. The most remarkable case of such selective nulling seen in our data is a significantly large number of nulls (≃6%) at lower frequencies, that are marked by the presence of a fairly narrow emission feature at the highest frequency of 4850 MHz. We refer to these as "low frequency (LF) nulls". We characterise the properties of high frequency (HF) emission at the occurrence of LF nulls, and compare and contrast them with that of "normal emission" at 4850 MHz. Our analysis shows that this high frequency emission tends to occur preferentially over a narrow range in longitude and with pulse widths typically of the order of a few milliseconds. We discuss the implications of our results for the pulsar emission mechanism in general and for the broadbandness of nulling phenomenon in particular. Our results signify the presence of an additional process of emission which does not turn off when the pulsar nulls at low frequencies, and becomes more prominent at higher frequencies. Our analysis also hints at a possible outer gap origin for this new population of pulses, and thus a likely connection to some high-energy emission processes that occur in the outer parts of the pulsar magnetosphere.</EA><CC>001E03</CC><FD>Observation simultanée; Observation radio; Pulsar radio; Observation multifréquence; Série temporelle; Dépendance fréquence; Magnétosphère stellaire; Rayonnement non thermique</FD><ED>Simultaneous observation; Radio observation; Radiopulsar; Multifrequency observation; Time series; Frequency dependence; Stellar magnetospheres; Nonthermal radiation</ED><SD>Observación simultánea; Observación radio; Pulsar radio; Observación multifrecuencia</SD><LO>INIST-14176.354000159602800300</LO><ID>07-0061207</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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