Fred's Contributions to Stellar Evolution
Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton...
Ausführliche Beschreibung
Autor*in: |
Mestel, L. [verfasserIn] |
---|
Format: |
Artikel |
---|---|
Sprache: |
Englisch |
Erschienen: |
2003 |
---|
Schlagwörter: |
---|
Anmerkung: |
© Kluwer Academic Publishers 2003 |
---|
Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Kluwer Academic Publishers, 1968, 285(2003), 2 vom: Juli, Seite 327-337 |
---|---|
Übergeordnetes Werk: |
volume:285 ; year:2003 ; number:2 ; month:07 ; pages:327-337 |
Links: |
---|
DOI / URN: |
10.1023/A:1025480207989 |
---|
Katalog-ID: |
OLC2066237795 |
---|
LEADER | 01000caa a22002652 4500 | ||
---|---|---|---|
001 | OLC2066237795 | ||
003 | DE-627 | ||
005 | 20230502213339.0 | ||
007 | tu | ||
008 | 200820s2003 xx ||||| 00| ||eng c | ||
024 | 7 | |a 10.1023/A:1025480207989 |2 doi | |
035 | |a (DE-627)OLC2066237795 | ||
035 | |a (DE-He213)A:1025480207989-p | ||
040 | |a DE-627 |b ger |c DE-627 |e rakwb | ||
041 | |a eng | ||
082 | 0 | 4 | |a 520 |a 530 |a 620 |q VZ |
084 | |a 16,12 |2 ssgn | ||
100 | 1 | |a Mestel, L. |e verfasserin |4 aut | |
245 | 1 | 0 | |a Fred's Contributions to Stellar Evolution |
264 | 1 | |c 2003 | |
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 2003 | ||
520 | |a Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars. | ||
650 | 4 | |a White Dwarf | |
650 | 4 | |a Main Sequence | |
650 | 4 | |a Stellar Evolution | |
650 | 4 | |a Main Sequence Star | |
650 | 4 | |a Stellar Structure | |
773 | 0 | 8 | |i Enthalten in |t Astrophysics and space science |d Kluwer Academic Publishers, 1968 |g 285(2003), 2 vom: Juli, Seite 327-337 |w (DE-627)129062723 |w (DE-600)629-4 |w (DE-576)014393522 |x 0004-640X |7 nnns |
773 | 1 | 8 | |g volume:285 |g year:2003 |g number:2 |g month:07 |g pages:327-337 |
856 | 4 | 1 | |u https://doi.org/10.1023/A:1025480207989 |z lizenzpflichtig |3 Volltext |
912 | |a GBV_USEFLAG_A | ||
912 | |a SYSFLAG_A | ||
912 | |a GBV_OLC | ||
912 | |a SSG-OLC-TEC | ||
912 | |a SSG-OLC-PHY | ||
912 | |a SSG-OLC-AST | ||
912 | |a SSG-OPC-AST | ||
912 | |a GBV_ILN_11 | ||
912 | |a GBV_ILN_40 | ||
912 | |a GBV_ILN_47 | ||
912 | |a GBV_ILN_70 | ||
912 | |a GBV_ILN_2002 | ||
912 | |a GBV_ILN_2279 | ||
912 | |a GBV_ILN_2286 | ||
912 | |a GBV_ILN_4012 | ||
951 | |a AR | ||
952 | |d 285 |j 2003 |e 2 |c 07 |h 327-337 |
author_variant |
l m lm |
---|---|
matchkey_str |
article:0004640X:2003----::rdcnrbtosotla |
hierarchy_sort_str |
2003 |
publishDate |
2003 |
allfields |
10.1023/A:1025480207989 doi (DE-627)OLC2066237795 (DE-He213)A:1025480207989-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Mestel, L. verfasserin aut Fred's Contributions to Stellar Evolution 2003 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2003 Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars. White Dwarf Main Sequence Stellar Evolution Main Sequence Star Stellar Structure Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 285(2003), 2 vom: Juli, Seite 327-337 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:285 year:2003 number:2 month:07 pages:327-337 https://doi.org/10.1023/A:1025480207989 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 285 2003 2 07 327-337 |
spelling |
10.1023/A:1025480207989 doi (DE-627)OLC2066237795 (DE-He213)A:1025480207989-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Mestel, L. verfasserin aut Fred's Contributions to Stellar Evolution 2003 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2003 Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars. White Dwarf Main Sequence Stellar Evolution Main Sequence Star Stellar Structure Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 285(2003), 2 vom: Juli, Seite 327-337 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:285 year:2003 number:2 month:07 pages:327-337 https://doi.org/10.1023/A:1025480207989 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 285 2003 2 07 327-337 |
allfields_unstemmed |
10.1023/A:1025480207989 doi (DE-627)OLC2066237795 (DE-He213)A:1025480207989-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Mestel, L. verfasserin aut Fred's Contributions to Stellar Evolution 2003 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2003 Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars. White Dwarf Main Sequence Stellar Evolution Main Sequence Star Stellar Structure Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 285(2003), 2 vom: Juli, Seite 327-337 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:285 year:2003 number:2 month:07 pages:327-337 https://doi.org/10.1023/A:1025480207989 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 285 2003 2 07 327-337 |
allfieldsGer |
10.1023/A:1025480207989 doi (DE-627)OLC2066237795 (DE-He213)A:1025480207989-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Mestel, L. verfasserin aut Fred's Contributions to Stellar Evolution 2003 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2003 Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars. White Dwarf Main Sequence Stellar Evolution Main Sequence Star Stellar Structure Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 285(2003), 2 vom: Juli, Seite 327-337 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:285 year:2003 number:2 month:07 pages:327-337 https://doi.org/10.1023/A:1025480207989 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 285 2003 2 07 327-337 |
allfieldsSound |
10.1023/A:1025480207989 doi (DE-627)OLC2066237795 (DE-He213)A:1025480207989-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Mestel, L. verfasserin aut Fred's Contributions to Stellar Evolution 2003 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 2003 Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars. White Dwarf Main Sequence Stellar Evolution Main Sequence Star Stellar Structure Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 285(2003), 2 vom: Juli, Seite 327-337 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:285 year:2003 number:2 month:07 pages:327-337 https://doi.org/10.1023/A:1025480207989 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 AR 285 2003 2 07 327-337 |
language |
English |
source |
Enthalten in Astrophysics and space science 285(2003), 2 vom: Juli, Seite 327-337 volume:285 year:2003 number:2 month:07 pages:327-337 |
sourceStr |
Enthalten in Astrophysics and space science 285(2003), 2 vom: Juli, Seite 327-337 volume:285 year:2003 number:2 month:07 pages:327-337 |
format_phy_str_mv |
Article |
institution |
findex.gbv.de |
topic_facet |
White Dwarf Main Sequence Stellar Evolution Main Sequence Star Stellar Structure |
dewey-raw |
520 |
isfreeaccess_bool |
false |
container_title |
Astrophysics and space science |
authorswithroles_txt_mv |
Mestel, L. @@aut@@ |
publishDateDaySort_date |
2003-07-01T00:00:00Z |
hierarchy_top_id |
129062723 |
dewey-sort |
3520 |
id |
OLC2066237795 |
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">OLC2066237795</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230502213339.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">200820s2003 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1023/A:1025480207989</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC2066237795</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-He213)A:1025480207989-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">520</subfield><subfield code="a">530</subfield><subfield code="a">620</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">Mestel, L.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Fred's Contributions to Stellar Evolution</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2003</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 2003</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">White Dwarf</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Main Sequence</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stellar Evolution</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Main Sequence Star</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stellar Structure</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Astrophysics and space science</subfield><subfield code="d">Kluwer Academic Publishers, 1968</subfield><subfield code="g">285(2003), 2 vom: Juli, Seite 327-337</subfield><subfield code="w">(DE-627)129062723</subfield><subfield code="w">(DE-600)629-4</subfield><subfield code="w">(DE-576)014393522</subfield><subfield code="x">0004-640X</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:285</subfield><subfield code="g">year:2003</subfield><subfield code="g">number:2</subfield><subfield code="g">month:07</subfield><subfield code="g">pages:327-337</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1023/A:1025480207989</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-TEC</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_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_2002</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2279</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2286</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4012</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">285</subfield><subfield code="j">2003</subfield><subfield code="e">2</subfield><subfield code="c">07</subfield><subfield code="h">327-337</subfield></datafield></record></collection>
|
author |
Mestel, L. |
spellingShingle |
Mestel, L. ddc 520 ssgn 16,12 misc White Dwarf misc Main Sequence misc Stellar Evolution misc Main Sequence Star misc Stellar Structure Fred's Contributions to Stellar Evolution |
authorStr |
Mestel, L. |
ppnlink_with_tag_str_mv |
@@773@@(DE-627)129062723 |
format |
Article |
dewey-ones |
520 - Astronomy & allied sciences 530 - Physics 620 - Engineering & allied operations |
delete_txt_mv |
keep |
author_role |
aut |
collection |
OLC |
remote_str |
false |
illustrated |
Not Illustrated |
issn |
0004-640X |
topic_title |
520 530 620 VZ 16,12 ssgn Fred's Contributions to Stellar Evolution White Dwarf Main Sequence Stellar Evolution Main Sequence Star Stellar Structure |
topic |
ddc 520 ssgn 16,12 misc White Dwarf misc Main Sequence misc Stellar Evolution misc Main Sequence Star misc Stellar Structure |
topic_unstemmed |
ddc 520 ssgn 16,12 misc White Dwarf misc Main Sequence misc Stellar Evolution misc Main Sequence Star misc Stellar Structure |
topic_browse |
ddc 520 ssgn 16,12 misc White Dwarf misc Main Sequence misc Stellar Evolution misc Main Sequence Star misc Stellar Structure |
format_facet |
Aufsätze Gedruckte Aufsätze |
format_main_str_mv |
Text Zeitschrift/Artikel |
carriertype_str_mv |
nc |
hierarchy_parent_title |
Astrophysics and space science |
hierarchy_parent_id |
129062723 |
dewey-tens |
520 - Astronomy 530 - Physics 620 - Engineering |
hierarchy_top_title |
Astrophysics and space science |
isfreeaccess_txt |
false |
familylinks_str_mv |
(DE-627)129062723 (DE-600)629-4 (DE-576)014393522 |
title |
Fred's Contributions to Stellar Evolution |
ctrlnum |
(DE-627)OLC2066237795 (DE-He213)A:1025480207989-p |
title_full |
Fred's Contributions to Stellar Evolution |
author_sort |
Mestel, L. |
journal |
Astrophysics and space science |
journalStr |
Astrophysics and space science |
lang_code |
eng |
isOA_bool |
false |
dewey-hundreds |
500 - Science 600 - Technology |
recordtype |
marc |
publishDateSort |
2003 |
contenttype_str_mv |
txt |
container_start_page |
327 |
author_browse |
Mestel, L. |
container_volume |
285 |
class |
520 530 620 VZ 16,12 ssgn |
format_se |
Aufsätze |
author-letter |
Mestel, L. |
doi_str_mv |
10.1023/A:1025480207989 |
dewey-full |
520 530 620 |
title_sort |
fred's contributions to stellar evolution |
title_auth |
Fred's Contributions to Stellar Evolution |
abstract |
Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars. © Kluwer Academic Publishers 2003 |
abstractGer |
Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars. © Kluwer Academic Publishers 2003 |
abstract_unstemmed |
Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars. © Kluwer Academic Publishers 2003 |
collection_details |
GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 |
container_issue |
2 |
title_short |
Fred's Contributions to Stellar Evolution |
url |
https://doi.org/10.1023/A:1025480207989 |
remote_bool |
false |
ppnlink |
129062723 |
mediatype_str_mv |
n |
isOA_txt |
false |
hochschulschrift_bool |
false |
doi_str |
10.1023/A:1025480207989 |
up_date |
2024-07-04T04:02:44.315Z |
_version_ |
1803619678883414016 |
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">OLC2066237795</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230502213339.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">200820s2003 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1023/A:1025480207989</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC2066237795</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-He213)A:1025480207989-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">520</subfield><subfield code="a">530</subfield><subfield code="a">620</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">Mestel, L.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Fred's Contributions to Stellar Evolution</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2003</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 2003</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract Fred began work on stellar structure after Hans Bethe and Carl-Friedrich von Weizsäcker had independently established that the thermonuclear fusion of hydrogen into helium is the primary source of the energy radiated by the Sun and other main sequence stars. A joint paper with Ray Lyttleton included this temperature-sensitive process explicitly in the energy equation, effectively vindicating the essentials of the theory of homogeneous gaseous stars presented in Sir Arthur Eddington's celebrated monograph `The Internal Constitution of the Stars'. Agreement with the solar luminosity can be obtained with two alternative values for the hydrogen content. In a subsequent paper, Fred argued convincingly in favour of the case with a very high rather than a moderate fraction of hydrogen. An epoch-making joint paper with Martin Schwarzschild followed the evolution of a low mass star through nuclear processing, from the main sequence into the giant domain in the Hertzsprung-Russell diagram. The slowly growing, burnt-out core becomes degenerate and nearly isothermal, while the photospheric boundary condition forces the expanding envelope to become largely convective. At the top of the giant branch, the degenerate core becomes hot enough for the fusion of helium into carbon; the consequent secular instability, noted first in studies of white dwarfs, brings the star down to the `horizontal branch', the location of the short-period globular cluster Cepheids. Two subsequent papers with Brian Haselgrove studied in further detail the structure of both main sequence and giant stars.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">White Dwarf</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Main Sequence</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stellar Evolution</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Main Sequence Star</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stellar Structure</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Astrophysics and space science</subfield><subfield code="d">Kluwer Academic Publishers, 1968</subfield><subfield code="g">285(2003), 2 vom: Juli, Seite 327-337</subfield><subfield code="w">(DE-627)129062723</subfield><subfield code="w">(DE-600)629-4</subfield><subfield code="w">(DE-576)014393522</subfield><subfield code="x">0004-640X</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:285</subfield><subfield code="g">year:2003</subfield><subfield code="g">number:2</subfield><subfield code="g">month:07</subfield><subfield code="g">pages:327-337</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1023/A:1025480207989</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-TEC</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_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_2002</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2279</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2286</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4012</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">285</subfield><subfield code="j">2003</subfield><subfield code="e">2</subfield><subfield code="c">07</subfield><subfield code="h">327-337</subfield></datafield></record></collection>
|
score |
7.400304 |