Determining the effective temperatures of G- and K-type giants and supergiants based on observed photometric indices
A method for determining the effective temperature T eff of G- and K-type giants and supergiants is proposed. The method is based on the use of two photometric indices free from the interstellar absorption influence: the Q index in the UBV photometric system and the [ c 1 ] index in the uvby system....
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| Veröffentlicht in: | Kinematics and physics of celestial bodies 2014-09, Vol.30 (5), p.244-254 |
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| container_title | Kinematics and physics of celestial bodies |
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| creator | Lyubimkov, L. S. Poklad, D. B. |
| description | A method for determining the effective temperature
T
eff
of G- and K-type giants and supergiants is proposed. The method is based on the use of two photometric indices free from the interstellar absorption influence: the
Q
index in the
UBV
photometric system and the [
c
1
] index in the
uvby
system. Empirical relations between the
T
eff
values found for nearby and bright G- and K-type giants and supergiants with the use of the infrared fluxes method (IRFM), on the one hand, and the observed
Q
and [
c
1
] indices for these stars, on the other hand, are plotted. A systematic discrepancy between the dependences of
T
eff
on
Q
for the stars with standard and reduced metallicities is found. Approximating the plotted dependences with second-order polynomials, one can obtain a relatively simple and a rather accurate method for determining the
T
eff
value in the range of 3800 ≤
T
≤ 5100 K (based on the
Q
index) or 4900 ≤
T
eff
≤ 5500 K (based on the [
c
1
] index). |
| doi_str_mv | 10.3103/S0884591314050055 |
| format | Article |
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T
eff
of G- and K-type giants and supergiants is proposed. The method is based on the use of two photometric indices free from the interstellar absorption influence: the
Q
index in the
UBV
photometric system and the [
c
1
] index in the
uvby
system. Empirical relations between the
T
eff
values found for nearby and bright G- and K-type giants and supergiants with the use of the infrared fluxes method (IRFM), on the one hand, and the observed
Q
and [
c
1
] indices for these stars, on the other hand, are plotted. A systematic discrepancy between the dependences of
T
eff
on
Q
for the stars with standard and reduced metallicities is found. Approximating the plotted dependences with second-order polynomials, one can obtain a relatively simple and a rather accurate method for determining the
T
eff
value in the range of 3800 ≤
T
≤ 5100 K (based on the
Q
index) or 4900 ≤
T
eff
≤ 5500 K (based on the [
c
1
] index).</description><identifier>ISSN: 0884-5913</identifier><identifier>EISSN: 1934-8401</identifier><identifier>DOI: 10.3103/S0884591314050055</identifier><language>eng</language><publisher>Heidelberg: Allerton Press</publisher><subject>Approximation ; Astronomy ; Giant stars ; Infrared ; Metallicity ; Observations and Techniques ; Photometry ; Physics ; Physics and Astronomy ; Physycs of Stars and Interstellar Medium ; Polynomials ; Stars ; Supergiant stars ; Temperature effects</subject><ispartof>Kinematics and physics of celestial bodies, 2014-09, Vol.30 (5), p.244-254</ispartof><rights>Allerton Press, Inc. 2014</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c382t-7bdf3912332db2baaafdbf3088c17b9cb48077daec4e8e725a26c9a43f92651e3</citedby><cites>FETCH-LOGICAL-c382t-7bdf3912332db2baaafdbf3088c17b9cb48077daec4e8e725a26c9a43f92651e3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.3103/S0884591314050055$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.3103/S0884591314050055$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,780,784,27924,27925,41488,42557,51319</link.rule.ids></links><search><creatorcontrib>Lyubimkov, L. S.</creatorcontrib><creatorcontrib>Poklad, D. B.</creatorcontrib><title>Determining the effective temperatures of G- and K-type giants and supergiants based on observed photometric indices</title><title>Kinematics and physics of celestial bodies</title><addtitle>Kinemat. Phys. Celest. Bodies</addtitle><description>A method for determining the effective temperature
T
eff
of G- and K-type giants and supergiants is proposed. The method is based on the use of two photometric indices free from the interstellar absorption influence: the
Q
index in the
UBV
photometric system and the [
c
1
] index in the
uvby
system. Empirical relations between the
T
eff
values found for nearby and bright G- and K-type giants and supergiants with the use of the infrared fluxes method (IRFM), on the one hand, and the observed
Q
and [
c
1
] indices for these stars, on the other hand, are plotted. A systematic discrepancy between the dependences of
T
eff
on
Q
for the stars with standard and reduced metallicities is found. Approximating the plotted dependences with second-order polynomials, one can obtain a relatively simple and a rather accurate method for determining the
T
eff
value in the range of 3800 ≤
T
≤ 5100 K (based on the
Q
index) or 4900 ≤
T
eff
≤ 5500 K (based on the [
c
1
] index).</description><subject>Approximation</subject><subject>Astronomy</subject><subject>Giant stars</subject><subject>Infrared</subject><subject>Metallicity</subject><subject>Observations and Techniques</subject><subject>Photometry</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Physycs of Stars and Interstellar Medium</subject><subject>Polynomials</subject><subject>Stars</subject><subject>Supergiant stars</subject><subject>Temperature effects</subject><issn>0884-5913</issn><issn>1934-8401</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GNUQQ</sourceid><recordid>eNqN0Utr3DAQB3BRGug26QfoTZBLL070tK1j2DYPspBDkrOR5dFGy1pyJXkh3z7abA6hJZCTHvP7DwyD0E9Kzjgl_PyetK2QinIqiCREyi9oQRUXVSsI_YoW-3K1r39D31PaFFEzJRYo_4YMcXTe-TXOT4DBWjDZ7QBnGCeIOs8REg4WX1VY-wHfVvl5Arx22uf0-pPm4t7evU4w4OBx6BPEXblPTyGHEXJ0Bjs_OAPpBB1ZvU3w4-08Ro-Xfx6W19Xq7upmebGqDG9Zrpp-sFxRxjkbetZrre3QW15GMbTplelFS5pm0GAEtNAwqVltlBbcKlZLCvwY_Tr0nWL4O0PK3eiSge1Wewhz6mgtGCeCt_ITlDGpVKOaQk__oZswR18GKYpK2taNEkXRgzIxpBTBdlN0o47PHSXdfmXdfysrGXbIpGL9GuK7zh-GXgBjQZjS</recordid><startdate>20140901</startdate><enddate>20140901</enddate><creator>Lyubimkov, L. 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B.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c382t-7bdf3912332db2baaafdbf3088c17b9cb48077daec4e8e725a26c9a43f92651e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2014</creationdate><topic>Approximation</topic><topic>Astronomy</topic><topic>Giant stars</topic><topic>Infrared</topic><topic>Metallicity</topic><topic>Observations and Techniques</topic><topic>Photometry</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Physycs of Stars and Interstellar Medium</topic><topic>Polynomials</topic><topic>Stars</topic><topic>Supergiant stars</topic><topic>Temperature effects</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Lyubimkov, L. S.</creatorcontrib><creatorcontrib>Poklad, D. 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S.</au><au>Poklad, D. B.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Determining the effective temperatures of G- and K-type giants and supergiants based on observed photometric indices</atitle><jtitle>Kinematics and physics of celestial bodies</jtitle><stitle>Kinemat. Phys. Celest. Bodies</stitle><date>2014-09-01</date><risdate>2014</risdate><volume>30</volume><issue>5</issue><spage>244</spage><epage>254</epage><pages>244-254</pages><issn>0884-5913</issn><eissn>1934-8401</eissn><abstract>A method for determining the effective temperature
T
eff
of G- and K-type giants and supergiants is proposed. The method is based on the use of two photometric indices free from the interstellar absorption influence: the
Q
index in the
UBV
photometric system and the [
c
1
] index in the
uvby
system. Empirical relations between the
T
eff
values found for nearby and bright G- and K-type giants and supergiants with the use of the infrared fluxes method (IRFM), on the one hand, and the observed
Q
and [
c
1
] indices for these stars, on the other hand, are plotted. A systematic discrepancy between the dependences of
T
eff
on
Q
for the stars with standard and reduced metallicities is found. Approximating the plotted dependences with second-order polynomials, one can obtain a relatively simple and a rather accurate method for determining the
T
eff
value in the range of 3800 ≤
T
≤ 5100 K (based on the
Q
index) or 4900 ≤
T
eff
≤ 5500 K (based on the [
c
1
] index).</abstract><cop>Heidelberg</cop><pub>Allerton Press</pub><doi>10.3103/S0884591314050055</doi><tpages>11</tpages></addata></record> |
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| ispartof | Kinematics and physics of celestial bodies, 2014-09, Vol.30 (5), p.244-254 |
| issn | 0884-5913 1934-8401 |
| language | eng |
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| source | SpringerNature Journals |
| subjects | Approximation Astronomy Giant stars Infrared Metallicity Observations and Techniques Photometry Physics Physics and Astronomy Physycs of Stars and Interstellar Medium Polynomials Stars Supergiant stars Temperature effects |
| title | Determining the effective temperatures of G- and K-type giants and supergiants based on observed photometric indices |
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