Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures
Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Vršnak, B. [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
2001 |
|---|
| Schlagwörter: |
|---|
| Anmerkung: |
© Kluwer Academic Publishers 2001 |
|---|
| Übergeordnetes Werk: |
Enthalten in: Solar physics - Kluwer Academic Publishers, 1967, 202(2001), 2 vom: Sept., Seite 319-335 |
|---|---|
| Übergeordnetes Werk: |
volume:202 ; year:2001 ; number:2 ; month:09 ; pages:319-335 |
| Links: |
|---|
| DOI / URN: |
10.1023/A:1012270414746 |
|---|
| Katalog-ID: |
OLC2033591964 |
|---|
| LEADER | 01000caa a22002652 4500 | ||
|---|---|---|---|
| 001 | OLC2033591964 | ||
| 003 | DE-627 | ||
| 005 | 20230504045658.0 | ||
| 007 | tu | ||
| 008 | 200819s2001 xx ||||| 00| ||eng c | ||
| 024 | 7 | |a 10.1023/A:1012270414746 |2 doi | |
| 035 | |a (DE-627)OLC2033591964 | ||
| 035 | |a (DE-He213)A:1012270414746-p | ||
| 040 | |a DE-627 |b ger |c DE-627 |e rakwb | ||
| 041 | |a eng | ||
| 082 | 0 | 4 | |a 530 |q VZ |
| 084 | |a 16,12 |2 ssgn | ||
| 100 | 1 | |a Vršnak, B. |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures |
| 264 | 1 | |c 2001 | |
| 336 | |a Text |b txt |2 rdacontent | ||
| 337 | |a ohne Hilfsmittel zu benutzen |b n |2 rdamedia | ||
| 338 | |a Band |b nc |2 rdacarrier | ||
| 500 | |a © Kluwer Academic Publishers 2001 | ||
| 520 | |a Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections. | ||
| 650 | 4 | |a Evaporation | |
| 650 | 4 | |a Microwave | |
| 650 | 4 | |a Comparative Analysis | |
| 650 | 4 | |a Flare | |
| 650 | 4 | |a Transition Region | |
| 700 | 1 | |a Magdalenić, J. |4 aut | |
| 700 | 1 | |a Aurass, H. |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Solar physics |d Kluwer Academic Publishers, 1967 |g 202(2001), 2 vom: Sept., Seite 319-335 |w (DE-627)129856010 |w (DE-600)281593-X |w (DE-576)015160033 |x 0038-0938 |7 nnns |
| 773 | 1 | 8 | |g volume:202 |g year:2001 |g number:2 |g month:09 |g pages:319-335 |
| 856 | 4 | 1 | |u https://doi.org/10.1023/A:1012270414746 |z lizenzpflichtig |3 Volltext |
| 912 | |a GBV_USEFLAG_A | ||
| 912 | |a SYSFLAG_A | ||
| 912 | |a GBV_OLC | ||
| 912 | |a SSG-OLC-PHY | ||
| 912 | |a SSG-OLC-AST | ||
| 912 | |a SSG-OPC-AST | ||
| 912 | |a GBV_ILN_11 | ||
| 912 | |a GBV_ILN_22 | ||
| 912 | |a GBV_ILN_40 | ||
| 912 | |a GBV_ILN_47 | ||
| 912 | |a GBV_ILN_70 | ||
| 912 | |a GBV_ILN_2286 | ||
| 951 | |a AR | ||
| 952 | |d 202 |j 2001 |e 2 |c 09 |h 319-335 | ||
| author_variant |
b v bv j m jm h a ha |
|---|---|
| matchkey_str |
article:00380938:2001----::oprtvaayiotpibrtadfhraadote |
| hierarchy_sort_str |
2001 |
| publishDate |
2001 |
| allfields |
10.1023/A:1012270414746 doi (DE-627)OLC2033591964 (DE-He213)A:1012270414746-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Vršnak, B. verfasserin aut Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures 2001 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2001 Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections. Evaporation Microwave Comparative Analysis Flare Transition Region Magdalenić, J. aut Aurass, H. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 202(2001), 2 vom: Sept., Seite 319-335 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:202 year:2001 number:2 month:09 pages:319-335 https://doi.org/10.1023/A:1012270414746 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2286 AR 202 2001 2 09 319-335 |
| spelling |
10.1023/A:1012270414746 doi (DE-627)OLC2033591964 (DE-He213)A:1012270414746-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Vršnak, B. verfasserin aut Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures 2001 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2001 Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections. Evaporation Microwave Comparative Analysis Flare Transition Region Magdalenić, J. aut Aurass, H. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 202(2001), 2 vom: Sept., Seite 319-335 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:202 year:2001 number:2 month:09 pages:319-335 https://doi.org/10.1023/A:1012270414746 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2286 AR 202 2001 2 09 319-335 |
| allfields_unstemmed |
10.1023/A:1012270414746 doi (DE-627)OLC2033591964 (DE-He213)A:1012270414746-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Vršnak, B. verfasserin aut Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures 2001 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2001 Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections. Evaporation Microwave Comparative Analysis Flare Transition Region Magdalenić, J. aut Aurass, H. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 202(2001), 2 vom: Sept., Seite 319-335 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:202 year:2001 number:2 month:09 pages:319-335 https://doi.org/10.1023/A:1012270414746 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2286 AR 202 2001 2 09 319-335 |
| allfieldsGer |
10.1023/A:1012270414746 doi (DE-627)OLC2033591964 (DE-He213)A:1012270414746-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Vršnak, B. verfasserin aut Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures 2001 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2001 Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections. Evaporation Microwave Comparative Analysis Flare Transition Region Magdalenić, J. aut Aurass, H. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 202(2001), 2 vom: Sept., Seite 319-335 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:202 year:2001 number:2 month:09 pages:319-335 https://doi.org/10.1023/A:1012270414746 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2286 AR 202 2001 2 09 319-335 |
| allfieldsSound |
10.1023/A:1012270414746 doi (DE-627)OLC2033591964 (DE-He213)A:1012270414746-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Vršnak, B. verfasserin aut Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures 2001 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2001 Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections. Evaporation Microwave Comparative Analysis Flare Transition Region Magdalenić, J. aut Aurass, H. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 202(2001), 2 vom: Sept., Seite 319-335 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:202 year:2001 number:2 month:09 pages:319-335 https://doi.org/10.1023/A:1012270414746 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2286 AR 202 2001 2 09 319-335 |
| language |
English |
| source |
Enthalten in Solar physics 202(2001), 2 vom: Sept., Seite 319-335 volume:202 year:2001 number:2 month:09 pages:319-335 |
| sourceStr |
Enthalten in Solar physics 202(2001), 2 vom: Sept., Seite 319-335 volume:202 year:2001 number:2 month:09 pages:319-335 |
| format_phy_str_mv |
Article |
| institution |
findex.gbv.de |
| topic_facet |
Evaporation Microwave Comparative Analysis Flare Transition Region |
| dewey-raw |
530 |
| isfreeaccess_bool |
false |
| container_title |
Solar physics |
| authorswithroles_txt_mv |
Vršnak, B. @@aut@@ Magdalenić, J. @@aut@@ Aurass, H. @@aut@@ |
| publishDateDaySort_date |
2001-09-01T00:00:00Z |
| hierarchy_top_id |
129856010 |
| dewey-sort |
3530 |
| id |
OLC2033591964 |
| language_de |
englisch |
| fullrecord |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">OLC2033591964</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230504045658.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">200819s2001 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1023/A:1012270414746</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC2033591964</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-He213)A:1012270414746-p</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="082" ind1="0" ind2="4"><subfield code="a">530</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">16,12</subfield><subfield code="2">ssgn</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Vršnak, B.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2001</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">ohne Hilfsmittel zu benutzen</subfield><subfield code="b">n</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Band</subfield><subfield code="b">nc</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">© Kluwer Academic Publishers 2001</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Evaporation</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Microwave</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Comparative Analysis</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Flare</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Transition Region</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Magdalenić, J.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Aurass, H.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Solar physics</subfield><subfield code="d">Kluwer Academic Publishers, 1967</subfield><subfield code="g">202(2001), 2 vom: Sept., Seite 319-335</subfield><subfield code="w">(DE-627)129856010</subfield><subfield code="w">(DE-600)281593-X</subfield><subfield code="w">(DE-576)015160033</subfield><subfield code="x">0038-0938</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:202</subfield><subfield code="g">year:2001</subfield><subfield code="g">number:2</subfield><subfield code="g">month:09</subfield><subfield code="g">pages:319-335</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1023/A:1012270414746</subfield><subfield code="z">lizenzpflichtig</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_OLC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHY</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_11</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_22</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_40</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_47</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_70</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2286</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">202</subfield><subfield code="j">2001</subfield><subfield code="e">2</subfield><subfield code="c">09</subfield><subfield code="h">319-335</subfield></datafield></record></collection>
|
| author |
Vršnak, B. |
| spellingShingle |
Vršnak, B. ddc 530 ssgn 16,12 misc Evaporation misc Microwave misc Comparative Analysis misc Flare misc Transition Region Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures |
| authorStr |
Vršnak, B. |
| ppnlink_with_tag_str_mv |
@@773@@(DE-627)129856010 |
| format |
Article |
| dewey-ones |
530 - Physics |
| delete_txt_mv |
keep |
| author_role |
aut aut aut |
| collection |
OLC |
| remote_str |
false |
| illustrated |
Not Illustrated |
| issn |
0038-0938 |
| topic_title |
530 VZ 16,12 ssgn Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures Evaporation Microwave Comparative Analysis Flare Transition Region |
| topic |
ddc 530 ssgn 16,12 misc Evaporation misc Microwave misc Comparative Analysis misc Flare misc Transition Region |
| topic_unstemmed |
ddc 530 ssgn 16,12 misc Evaporation misc Microwave misc Comparative Analysis misc Flare misc Transition Region |
| topic_browse |
ddc 530 ssgn 16,12 misc Evaporation misc Microwave misc Comparative Analysis misc Flare misc Transition Region |
| format_facet |
Aufsätze Gedruckte Aufsätze |
| format_main_str_mv |
Text Zeitschrift/Artikel |
| carriertype_str_mv |
nc |
| hierarchy_parent_title |
Solar physics |
| hierarchy_parent_id |
129856010 |
| dewey-tens |
530 - Physics |
| hierarchy_top_title |
Solar physics |
| isfreeaccess_txt |
false |
| familylinks_str_mv |
(DE-627)129856010 (DE-600)281593-X (DE-576)015160033 |
| title |
Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures |
| ctrlnum |
(DE-627)OLC2033591964 (DE-He213)A:1012270414746-p |
| title_full |
Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures |
| author_sort |
Vršnak, B. |
| journal |
Solar physics |
| journalStr |
Solar physics |
| lang_code |
eng |
| isOA_bool |
false |
| dewey-hundreds |
500 - Science |
| recordtype |
marc |
| publishDateSort |
2001 |
| contenttype_str_mv |
txt |
| container_start_page |
319 |
| author_browse |
Vršnak, B. Magdalenić, J. Aurass, H. |
| container_volume |
202 |
| class |
530 VZ 16,12 ssgn |
| format_se |
Aufsätze |
| author-letter |
Vršnak, B. |
| doi_str_mv |
10.1023/A:1012270414746 |
| dewey-full |
530 |
| title_sort |
comparative analysis of type ii bursts and of thermal and non-thermal flare signatures |
| title_auth |
Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures |
| abstract |
Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections. © Kluwer Academic Publishers 2001 |
| abstractGer |
Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections. © Kluwer Academic Publishers 2001 |
| abstract_unstemmed |
Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections. © Kluwer Academic Publishers 2001 |
| collection_details |
GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2286 |
| container_issue |
2 |
| title_short |
Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures |
| url |
https://doi.org/10.1023/A:1012270414746 |
| remote_bool |
false |
| author2 |
Magdalenić, J. Aurass, H. |
| author2Str |
Magdalenić, J. Aurass, H. |
| ppnlink |
129856010 |
| mediatype_str_mv |
n |
| isOA_txt |
false |
| hochschulschrift_bool |
false |
| doi_str |
10.1023/A:1012270414746 |
| up_date |
2024-07-03T17:36:13.966Z |
| _version_ |
1803580262546669568 |
| fullrecord_marcxml |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">OLC2033591964</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230504045658.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">200819s2001 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1023/A:1012270414746</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC2033591964</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-He213)A:1012270414746-p</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="082" ind1="0" ind2="4"><subfield code="a">530</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">16,12</subfield><subfield code="2">ssgn</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Vršnak, B.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Comparative Analysis of Type ii Bursts and of Thermal and non-Thermal Flare Signatures</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2001</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">ohne Hilfsmittel zu benutzen</subfield><subfield code="b">n</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Band</subfield><subfield code="b">nc</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">© Kluwer Academic Publishers 2001</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract The relationship between metric type II radio bursts and solar flares is studied. Well-defined correlations between the properties of type II bursts and the characteristics of associated microwave and soft X-ray bursts are established in two entirely independent data sets. It is shown that the correlations are strongly affected by the wide range of coronal Alfvén velocities involved, comprising values from only 150 up to 800 km $ s^{−1} $, with a typical value of 400 km $ s^{−1} $. After careful data analysis it was inferred that type II bursts are more closely related to the soft X-ray bursts than they are to microwave bursts. The correlations indicate that type II burst shocks are preferably generated by flares with a relatively strong thermal component, and that the shocks are probably ignited by the plasma expansion associated with the 'evaporation' process in the transition region. Although the results imply that the majority of metric type II bursts are caused by flares, a simple geometrical consideration shows that a fraction of non-flare type II bursts cannot be explained by behind-limb events and that roughly 10% of metric type II bursts should be attributed to non-flare coronal mass ejections.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Evaporation</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Microwave</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Comparative Analysis</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Flare</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Transition Region</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Magdalenić, J.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Aurass, H.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Solar physics</subfield><subfield code="d">Kluwer Academic Publishers, 1967</subfield><subfield code="g">202(2001), 2 vom: Sept., Seite 319-335</subfield><subfield code="w">(DE-627)129856010</subfield><subfield code="w">(DE-600)281593-X</subfield><subfield code="w">(DE-576)015160033</subfield><subfield code="x">0038-0938</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:202</subfield><subfield code="g">year:2001</subfield><subfield code="g">number:2</subfield><subfield code="g">month:09</subfield><subfield code="g">pages:319-335</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1023/A:1012270414746</subfield><subfield code="z">lizenzpflichtig</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_OLC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHY</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_11</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_22</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_40</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_47</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_70</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2286</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">202</subfield><subfield code="j">2001</subfield><subfield code="e">2</subfield><subfield code="c">09</subfield><subfield code="h">319-335</subfield></datafield></record></collection>
|
| score |
7.401457 |