Three years of photometry of IM Pegasi = HR 8703
Differential photometry of this K1 IV-III p RS CVn-type binary in 1978-79, 1979-80, and 1980-81 at eight different observatories shows that the variability, discovered originally by Herbst, is periodic. The mean of three different determinations of the photometric period was 24(d).39 + or 0(d).03, a...
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| Veröffentlicht in: | Astrophysics and space science 1983-01, Vol.89 (1 Ja), p.53-60 |
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| container_title | Astrophysics and space science |
| container_volume | 89 |
| creator | Eaton, J. A. Hall, D. S. Henry, G. W. Lovell, L. P. Stephan, C. A. Chambliss, C. R. Detterline, P. K. Landis, H. J. Louth, H. Renner, T. R. |
| description | Differential photometry of this K1 IV-III p RS CVn-type binary in 1978-79, 1979-80, and 1980-81 at eight different observatories shows that the variability, discovered originally by Herbst, is periodic. The mean of three different determinations of the photometric period was 24(d).39 + or 0(d).03, about 1 percent shorter than the orbital period of 24(d).649 determined spectroscopically by Harper. The total range observed during these three years was for V from 5(m).60 to 5(m).85. The light curve was nearly sinusoidal but always noticieably asymmetric, with the sense reversing sometime between 1979-80 and 1980-81. |
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A. ; Hall, D. S. ; Henry, G. W. ; Lovell, L. P. ; Stephan, C. A. ; Chambliss, C. R. ; Detterline, P. K. ; Landis, H. J. ; Louth, H. ; Renner, T. R.</creator><creatorcontrib>Eaton, J. A. ; Hall, D. S. ; Henry, G. W. ; Lovell, L. P. ; Stephan, C. A. ; Chambliss, C. R. ; Detterline, P. K. ; Landis, H. J. ; Louth, H. ; Renner, T. R.</creatorcontrib><description>Differential photometry of this K1 IV-III p RS CVn-type binary in 1978-79, 1979-80, and 1980-81 at eight different observatories shows that the variability, discovered originally by Herbst, is periodic. The mean of three different determinations of the photometric period was 24(d).39 + or 0(d).03, about 1 percent shorter than the orbital period of 24(d).649 determined spectroscopically by Harper. The total range observed during these three years was for V from 5(m).60 to 5(m).85. The light curve was nearly sinusoidal but always noticieably asymmetric, with the sense reversing sometime between 1979-80 and 1980-81.</description><identifier>ISSN: 0004-640X</identifier><language>eng</language><publisher>Legacy CDMS</publisher><subject>Astronomy</subject><ispartof>Astrophysics and space science, 1983-01, Vol.89 (1 Ja), p.53-60</ispartof><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784</link.rule.ids></links><search><creatorcontrib>Eaton, J. A.</creatorcontrib><creatorcontrib>Hall, D. S.</creatorcontrib><creatorcontrib>Henry, G. W.</creatorcontrib><creatorcontrib>Lovell, L. P.</creatorcontrib><creatorcontrib>Stephan, C. A.</creatorcontrib><creatorcontrib>Chambliss, C. R.</creatorcontrib><creatorcontrib>Detterline, P. K.</creatorcontrib><creatorcontrib>Landis, H. J.</creatorcontrib><creatorcontrib>Louth, H.</creatorcontrib><creatorcontrib>Renner, T. R.</creatorcontrib><title>Three years of photometry of IM Pegasi = HR 8703</title><title>Astrophysics and space science</title><description>Differential photometry of this K1 IV-III p RS CVn-type binary in 1978-79, 1979-80, and 1980-81 at eight different observatories shows that the variability, discovered originally by Herbst, is periodic. The mean of three different determinations of the photometric period was 24(d).39 + or 0(d).03, about 1 percent shorter than the orbital period of 24(d).649 determined spectroscopically by Harper. The total range observed during these three years was for V from 5(m).60 to 5(m).85. 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P.</creatorcontrib><creatorcontrib>Stephan, C. A.</creatorcontrib><creatorcontrib>Chambliss, C. R.</creatorcontrib><creatorcontrib>Detterline, P. K.</creatorcontrib><creatorcontrib>Landis, H. J.</creatorcontrib><creatorcontrib>Louth, H.</creatorcontrib><creatorcontrib>Renner, T. R.</creatorcontrib><collection>NASA Scientific and Technical Information</collection><collection>NASA Technical Reports Server</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astrophysics and space science</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Eaton, J. A.</au><au>Hall, D. S.</au><au>Henry, G. W.</au><au>Lovell, L. P.</au><au>Stephan, C. A.</au><au>Chambliss, C. R.</au><au>Detterline, P. K.</au><au>Landis, H. J.</au><au>Louth, H.</au><au>Renner, T. R.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Three years of photometry of IM Pegasi = HR 8703</atitle><jtitle>Astrophysics and space science</jtitle><date>1983-01-01</date><risdate>1983</risdate><volume>89</volume><issue>1 Ja</issue><spage>53</spage><epage>60</epage><pages>53-60</pages><issn>0004-640X</issn><abstract>Differential photometry of this K1 IV-III p RS CVn-type binary in 1978-79, 1979-80, and 1980-81 at eight different observatories shows that the variability, discovered originally by Herbst, is periodic. The mean of three different determinations of the photometric period was 24(d).39 + or 0(d).03, about 1 percent shorter than the orbital period of 24(d).649 determined spectroscopically by Harper. The total range observed during these three years was for V from 5(m).60 to 5(m).85. 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| ispartof | Astrophysics and space science, 1983-01, Vol.89 (1 Ja), p.53-60 |
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| language | eng |
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| source | NASA Technical Reports Server; EZB-FREE-00999 freely available EZB journals; SpringerLink Journals - AutoHoldings |
| subjects | Astronomy |
| title | Three years of photometry of IM Pegasi = HR 8703 |
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