Influence of α-enhancement on effective temperatures of hot subdwarfs
Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to expla...
Ausführliche Beschreibung
Autor*in: |
Guo, Jianpo [verfasserIn] |
---|
Format: |
Artikel |
---|---|
Sprache: |
Englisch |
Erschienen: |
2010 |
---|
Schlagwörter: |
---|
Anmerkung: |
© Springer Science+Business Media B.V. 2010 |
---|
Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Springer Netherlands, 1968, 329(2010), 1-2 vom: 12. Feb., Seite 15-18 |
---|---|
Übergeordnetes Werk: |
volume:329 ; year:2010 ; number:1-2 ; day:12 ; month:02 ; pages:15-18 |
Links: |
---|
DOI / URN: |
10.1007/s10509-010-0291-4 |
---|
Katalog-ID: |
OLC2066259497 |
---|
LEADER | 01000caa a22002652 4500 | ||
---|---|---|---|
001 | OLC2066259497 | ||
003 | DE-627 | ||
005 | 20230502213621.0 | ||
007 | tu | ||
008 | 200820s2010 xx ||||| 00| ||eng c | ||
024 | 7 | |a 10.1007/s10509-010-0291-4 |2 doi | |
035 | |a (DE-627)OLC2066259497 | ||
035 | |a (DE-He213)s10509-010-0291-4-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 Guo, Jianpo |e verfasserin |4 aut | |
245 | 1 | 0 | |a Influence of α-enhancement on effective temperatures of hot subdwarfs |
264 | 1 | |c 2010 | |
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 © Springer Science+Business Media B.V. 2010 | ||
520 | |a Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is. | ||
650 | 4 | |a Stars: abundances | |
650 | 4 | |a Stars: subdwarfs | |
650 | 4 | |a Stars: horizontal-branch | |
700 | 1 | |a Zhang, Fenghui |4 aut | |
700 | 1 | |a Zhang, Xianfei |4 aut | |
700 | 1 | |a Han, Zhanwen |4 aut | |
773 | 0 | 8 | |i Enthalten in |t Astrophysics and space science |d Springer Netherlands, 1968 |g 329(2010), 1-2 vom: 12. Feb., Seite 15-18 |w (DE-627)129062723 |w (DE-600)629-4 |w (DE-576)014393522 |x 0004-640X |7 nnns |
773 | 1 | 8 | |g volume:329 |g year:2010 |g number:1-2 |g day:12 |g month:02 |g pages:15-18 |
856 | 4 | 1 | |u https://doi.org/10.1007/s10509-010-0291-4 |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_40 | ||
912 | |a GBV_ILN_47 | ||
912 | |a GBV_ILN_70 | ||
912 | |a GBV_ILN_2279 | ||
912 | |a GBV_ILN_4012 | ||
951 | |a AR | ||
952 | |d 329 |j 2010 |e 1-2 |b 12 |c 02 |h 15-18 |
author_variant |
j g jg f z fz x z xz z h zh |
---|---|
matchkey_str |
article:0004640X:2010----::nlecoehneetnfetvtmeau |
hierarchy_sort_str |
2010 |
publishDate |
2010 |
allfields |
10.1007/s10509-010-0291-4 doi (DE-627)OLC2066259497 (DE-He213)s10509-010-0291-4-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Guo, Jianpo verfasserin aut Influence of α-enhancement on effective temperatures of hot subdwarfs 2010 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media B.V. 2010 Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is. Stars: abundances Stars: subdwarfs Stars: horizontal-branch Zhang, Fenghui aut Zhang, Xianfei aut Han, Zhanwen aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 329(2010), 1-2 vom: 12. Feb., Seite 15-18 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:329 year:2010 number:1-2 day:12 month:02 pages:15-18 https://doi.org/10.1007/s10509-010-0291-4 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 329 2010 1-2 12 02 15-18 |
spelling |
10.1007/s10509-010-0291-4 doi (DE-627)OLC2066259497 (DE-He213)s10509-010-0291-4-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Guo, Jianpo verfasserin aut Influence of α-enhancement on effective temperatures of hot subdwarfs 2010 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media B.V. 2010 Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is. Stars: abundances Stars: subdwarfs Stars: horizontal-branch Zhang, Fenghui aut Zhang, Xianfei aut Han, Zhanwen aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 329(2010), 1-2 vom: 12. Feb., Seite 15-18 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:329 year:2010 number:1-2 day:12 month:02 pages:15-18 https://doi.org/10.1007/s10509-010-0291-4 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 329 2010 1-2 12 02 15-18 |
allfields_unstemmed |
10.1007/s10509-010-0291-4 doi (DE-627)OLC2066259497 (DE-He213)s10509-010-0291-4-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Guo, Jianpo verfasserin aut Influence of α-enhancement on effective temperatures of hot subdwarfs 2010 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media B.V. 2010 Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is. Stars: abundances Stars: subdwarfs Stars: horizontal-branch Zhang, Fenghui aut Zhang, Xianfei aut Han, Zhanwen aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 329(2010), 1-2 vom: 12. Feb., Seite 15-18 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:329 year:2010 number:1-2 day:12 month:02 pages:15-18 https://doi.org/10.1007/s10509-010-0291-4 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 329 2010 1-2 12 02 15-18 |
allfieldsGer |
10.1007/s10509-010-0291-4 doi (DE-627)OLC2066259497 (DE-He213)s10509-010-0291-4-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Guo, Jianpo verfasserin aut Influence of α-enhancement on effective temperatures of hot subdwarfs 2010 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media B.V. 2010 Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is. Stars: abundances Stars: subdwarfs Stars: horizontal-branch Zhang, Fenghui aut Zhang, Xianfei aut Han, Zhanwen aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 329(2010), 1-2 vom: 12. Feb., Seite 15-18 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:329 year:2010 number:1-2 day:12 month:02 pages:15-18 https://doi.org/10.1007/s10509-010-0291-4 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 329 2010 1-2 12 02 15-18 |
allfieldsSound |
10.1007/s10509-010-0291-4 doi (DE-627)OLC2066259497 (DE-He213)s10509-010-0291-4-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Guo, Jianpo verfasserin aut Influence of α-enhancement on effective temperatures of hot subdwarfs 2010 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media B.V. 2010 Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is. Stars: abundances Stars: subdwarfs Stars: horizontal-branch Zhang, Fenghui aut Zhang, Xianfei aut Han, Zhanwen aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 329(2010), 1-2 vom: 12. Feb., Seite 15-18 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:329 year:2010 number:1-2 day:12 month:02 pages:15-18 https://doi.org/10.1007/s10509-010-0291-4 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 329 2010 1-2 12 02 15-18 |
language |
English |
source |
Enthalten in Astrophysics and space science 329(2010), 1-2 vom: 12. Feb., Seite 15-18 volume:329 year:2010 number:1-2 day:12 month:02 pages:15-18 |
sourceStr |
Enthalten in Astrophysics and space science 329(2010), 1-2 vom: 12. Feb., Seite 15-18 volume:329 year:2010 number:1-2 day:12 month:02 pages:15-18 |
format_phy_str_mv |
Article |
institution |
findex.gbv.de |
topic_facet |
Stars: abundances Stars: subdwarfs Stars: horizontal-branch |
dewey-raw |
520 |
isfreeaccess_bool |
false |
container_title |
Astrophysics and space science |
authorswithroles_txt_mv |
Guo, Jianpo @@aut@@ Zhang, Fenghui @@aut@@ Zhang, Xianfei @@aut@@ Han, Zhanwen @@aut@@ |
publishDateDaySort_date |
2010-02-12T00:00:00Z |
hierarchy_top_id |
129062723 |
dewey-sort |
3520 |
id |
OLC2066259497 |
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">OLC2066259497</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230502213621.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">200820s2010 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/s10509-010-0291-4</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC2066259497</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-He213)s10509-010-0291-4-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">Guo, Jianpo</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Influence of α-enhancement on effective temperatures of hot subdwarfs</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2010</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">© Springer Science+Business Media B.V. 2010</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stars: abundances</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stars: subdwarfs</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stars: horizontal-branch</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Zhang, Fenghui</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Zhang, Xianfei</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Han, Zhanwen</subfield><subfield code="4">aut</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">Springer Netherlands, 1968</subfield><subfield code="g">329(2010), 1-2 vom: 12. Feb., Seite 15-18</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:329</subfield><subfield code="g">year:2010</subfield><subfield code="g">number:1-2</subfield><subfield code="g">day:12</subfield><subfield code="g">month:02</subfield><subfield code="g">pages:15-18</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1007/s10509-010-0291-4</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_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_2279</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">329</subfield><subfield code="j">2010</subfield><subfield code="e">1-2</subfield><subfield code="b">12</subfield><subfield code="c">02</subfield><subfield code="h">15-18</subfield></datafield></record></collection>
|
author |
Guo, Jianpo |
spellingShingle |
Guo, Jianpo ddc 520 ssgn 16,12 misc Stars: abundances misc Stars: subdwarfs misc Stars: horizontal-branch Influence of α-enhancement on effective temperatures of hot subdwarfs |
authorStr |
Guo, Jianpo |
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 aut aut aut |
collection |
OLC |
remote_str |
false |
illustrated |
Not Illustrated |
issn |
0004-640X |
topic_title |
520 530 620 VZ 16,12 ssgn Influence of α-enhancement on effective temperatures of hot subdwarfs Stars: abundances Stars: subdwarfs Stars: horizontal-branch |
topic |
ddc 520 ssgn 16,12 misc Stars: abundances misc Stars: subdwarfs misc Stars: horizontal-branch |
topic_unstemmed |
ddc 520 ssgn 16,12 misc Stars: abundances misc Stars: subdwarfs misc Stars: horizontal-branch |
topic_browse |
ddc 520 ssgn 16,12 misc Stars: abundances misc Stars: subdwarfs misc Stars: horizontal-branch |
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 |
Influence of α-enhancement on effective temperatures of hot subdwarfs |
ctrlnum |
(DE-627)OLC2066259497 (DE-He213)s10509-010-0291-4-p |
title_full |
Influence of α-enhancement on effective temperatures of hot subdwarfs |
author_sort |
Guo, Jianpo |
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 |
2010 |
contenttype_str_mv |
txt |
container_start_page |
15 |
author_browse |
Guo, Jianpo Zhang, Fenghui Zhang, Xianfei Han, Zhanwen |
container_volume |
329 |
class |
520 530 620 VZ 16,12 ssgn |
format_se |
Aufsätze |
author-letter |
Guo, Jianpo |
doi_str_mv |
10.1007/s10509-010-0291-4 |
dewey-full |
520 530 620 |
title_sort |
influence of α-enhancement on effective temperatures of hot subdwarfs |
title_auth |
Influence of α-enhancement on effective temperatures of hot subdwarfs |
abstract |
Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is. © Springer Science+Business Media B.V. 2010 |
abstractGer |
Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is. © Springer Science+Business Media B.V. 2010 |
abstract_unstemmed |
Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is. © Springer Science+Business Media B.V. 2010 |
collection_details |
GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 |
container_issue |
1-2 |
title_short |
Influence of α-enhancement on effective temperatures of hot subdwarfs |
url |
https://doi.org/10.1007/s10509-010-0291-4 |
remote_bool |
false |
author2 |
Zhang, Fenghui Zhang, Xianfei Han, Zhanwen |
author2Str |
Zhang, Fenghui Zhang, Xianfei Han, Zhanwen |
ppnlink |
129062723 |
mediatype_str_mv |
n |
isOA_txt |
false |
hochschulschrift_bool |
false |
doi_str |
10.1007/s10509-010-0291-4 |
up_date |
2024-07-04T04:05:40.681Z |
_version_ |
1803619863816568832 |
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">OLC2066259497</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230502213621.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">200820s2010 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/s10509-010-0291-4</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC2066259497</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-He213)s10509-010-0291-4-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">Guo, Jianpo</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Influence of α-enhancement on effective temperatures of hot subdwarfs</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2010</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">© Springer Science+Business Media B.V. 2010</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract Observations of metal elements in some halo or bulge globular clusters and in some elliptical galaxies have shown the α-enhancement phenomenon. Hot subdwarfs are important stars, e.g., they are important sources of far-ultraviolet light in the Galaxy and have successfully been used to explain the UV-upturn in elliptical galaxies. Therefore, we try to study the impacts of α-enhancement on hot subdwarfs. In our calculation, the value of the metallicity is 0.02, all the core masses of hot subdwarfs are 0.475 M⊙, and the envelope masses of the hot subdwarfs are 0.001, 0.005 and 0.016 M⊙, respectively. We find that the influences of α-enhancement on luminosity and evolutionary age of hot subdwarfs are not visible. But α-enhancement can make the effective temperatures of hot subdwarfs become higher, and the thicker their envelopes are, the more obvious this influence is.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stars: abundances</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stars: subdwarfs</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stars: horizontal-branch</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Zhang, Fenghui</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Zhang, Xianfei</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Han, Zhanwen</subfield><subfield code="4">aut</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">Springer Netherlands, 1968</subfield><subfield code="g">329(2010), 1-2 vom: 12. Feb., Seite 15-18</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:329</subfield><subfield code="g">year:2010</subfield><subfield code="g">number:1-2</subfield><subfield code="g">day:12</subfield><subfield code="g">month:02</subfield><subfield code="g">pages:15-18</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1007/s10509-010-0291-4</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_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_2279</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">329</subfield><subfield code="j">2010</subfield><subfield code="e">1-2</subfield><subfield code="b">12</subfield><subfield code="c">02</subfield><subfield code="h">15-18</subfield></datafield></record></collection>
|
score |
7.4004126 |