Fine structures in time profiles of type II bursts at frequencies above 200 MHz
Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in dif...
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| Autor*in: |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
1993 |
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| Umfang: |
12 |
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| Reproduktion: |
Springer Online Journal Archives 1860-2002 |
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| Übergeordnetes Werk: |
in: Solar physics - 1967, 144(1993) vom: Feb., Seite 373-384 |
| Übergeordnetes Werk: |
volume:144 ; year:1993 ; month:02 ; pages:373-384 ; extent:12 |
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NLEJ195846966 |
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| 520 | |a Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event. At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts. The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983). | ||
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| 700 | 1 | |a Messerotti, M. |4 oth | |
| 700 | 1 | |a Karlický, M. |4 oth | |
| 700 | 1 | |a Urbarz, H. |4 oth | |
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(DE-627)NLEJ195846966 DE-627 ger DE-627 rakwb eng Fine structures in time profiles of type II bursts at frequencies above 200 MHz 1993 12 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event. At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts. The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983). Springer Online Journal Archives 1860-2002 Zlobec, P. oth Messerotti, M. oth Karlický, M. oth Urbarz, H. oth in Solar physics 1967 144(1993) vom: Feb., Seite 373-384 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:144 year:1993 month:02 pages:373-384 extent:12 http://dx.doi.org/10.1007/BF00627601 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 144 1993 2 373-384 12 |
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(DE-627)NLEJ195846966 DE-627 ger DE-627 rakwb eng Fine structures in time profiles of type II bursts at frequencies above 200 MHz 1993 12 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event. At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts. The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983). Springer Online Journal Archives 1860-2002 Zlobec, P. oth Messerotti, M. oth Karlický, M. oth Urbarz, H. oth in Solar physics 1967 144(1993) vom: Feb., Seite 373-384 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:144 year:1993 month:02 pages:373-384 extent:12 http://dx.doi.org/10.1007/BF00627601 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 144 1993 2 373-384 12 |
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(DE-627)NLEJ195846966 DE-627 ger DE-627 rakwb eng Fine structures in time profiles of type II bursts at frequencies above 200 MHz 1993 12 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event. At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts. The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983). Springer Online Journal Archives 1860-2002 Zlobec, P. oth Messerotti, M. oth Karlický, M. oth Urbarz, H. oth in Solar physics 1967 144(1993) vom: Feb., Seite 373-384 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:144 year:1993 month:02 pages:373-384 extent:12 http://dx.doi.org/10.1007/BF00627601 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 144 1993 2 373-384 12 |
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(DE-627)NLEJ195846966 DE-627 ger DE-627 rakwb eng Fine structures in time profiles of type II bursts at frequencies above 200 MHz 1993 12 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event. At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts. The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983). Springer Online Journal Archives 1860-2002 Zlobec, P. oth Messerotti, M. oth Karlický, M. oth Urbarz, H. oth in Solar physics 1967 144(1993) vom: Feb., Seite 373-384 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:144 year:1993 month:02 pages:373-384 extent:12 http://dx.doi.org/10.1007/BF00627601 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 144 1993 2 373-384 12 |
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(DE-627)NLEJ195846966 DE-627 ger DE-627 rakwb eng Fine structures in time profiles of type II bursts at frequencies above 200 MHz 1993 12 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event. At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts. The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983). Springer Online Journal Archives 1860-2002 Zlobec, P. oth Messerotti, M. oth Karlický, M. oth Urbarz, H. oth in Solar physics 1967 144(1993) vom: Feb., Seite 373-384 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:144 year:1993 month:02 pages:373-384 extent:12 http://dx.doi.org/10.1007/BF00627601 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 144 1993 2 373-384 12 |
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Fine structures in time profiles of type II bursts at frequencies above 200 MHz |
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Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event. At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts. The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983). |
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Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event. At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts. The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983). |
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Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event. At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts. The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983). |
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<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">NLEJ195846966</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20210708014750.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">070526s1993 xx |||||o 00| ||eng c</controlfield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)NLEJ195846966</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Fine structures in time profiles of type II bursts at frequencies above 200 MHz</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">1993</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">12</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zzz</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">z</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zu</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz. The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event. At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts. The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983).</subfield></datafield><datafield tag="533" ind1=" " ind2=" "><subfield code="f">Springer Online Journal Archives 1860-2002</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Zlobec, P.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Messerotti, M.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Karlický, M.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Urbarz, H.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">in</subfield><subfield code="t">Solar physics</subfield><subfield code="d">1967</subfield><subfield code="g">144(1993) vom: Feb., Seite 373-384</subfield><subfield code="w">(DE-627)NLEJ188983465</subfield><subfield code="w">(DE-600)1473830-2</subfield><subfield code="x">1573-093X</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:144</subfield><subfield code="g">year:1993</subfield><subfield code="g">month:02</subfield><subfield code="g">pages:373-384</subfield><subfield code="g">extent:12</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">http://dx.doi.org/10.1007/BF00627601</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_U</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">ZDB-1-SOJ</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_NL_ARTICLE</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">144</subfield><subfield code="j">1993</subfield><subfield code="c">2</subfield><subfield code="h">373-384</subfield><subfield code="g">12</subfield></datafield></record></collection>
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