Kepler photometry of the prototypical Blazhko star RR Lyr: an old friend seen in a new light
Identifieur interne : 001F91 ( PascalFrancis/Corpus ); précédent : 001F90; suivant : 001F92Kepler photometry of the prototypical Blazhko star RR Lyr: an old friend seen in a new light
Auteurs : K. Kolenberg ; S. Bryson ; R. Szabo ; D. W. Kurtz ; R. Smolec ; J. M. Nemec ; E. Guggenberger ; P. Moskalik ; J. M. Benkö ; M. Chadid ; Y.-B. Jeon ; L. L. Kiss ; G. Kopacki ; J. Nuspl ; M. Still ; J. Christensen-Dalsgaard ; H. Kjeldsen ; W. J. Borucki ; D. A. Caldwell ; J. M. Jenkins ; D. KochSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.
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Abstract
We present our analysis of the long-cadence Kepler data for the well-studied Blazhko star RR Lyr, gathered during the first two quarters of the satellite's observations and covering a total of 127 d. Besides being of great importance for our understanding of RR Lyrae stars in general, these RR Lyr data can be regarded as a case study for observations of bright stars with Kepler. Kepler can perform high-precision photometry on targets like RR Lyr, as the saturated flux is conserved to a very high degree. The Kepler data on RR Lyr are revolutionary in several respects. Even with long-cadence sampling (one measurement per 29.4 min), the unprecedented precision (< mmag) of the Kepler photometry allows the study of the star's extreme light-curve variations in detail. The multiplet structures at the main frequency and its harmonics, typical for Blazhko stars, are clearly detected up to the quintuplets. For the first time, photometric data of RR Lyr reveal the presence of half-integer frequencies, linked to a period-doubling effect. This phenomenon may be connected to the still unexplained Blazhko modulation. Moreover, with three observed Blazhko cycles at our disposal, we observe that there is no exact repetition in the light-curve changes from one modulation cycle to the next for RR Lyr. This may be due to additional periodicities in the star, or to transient or quasi-periodic changes.
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| NO : | PASCAL 11-0114653 INIST |
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| ET : | Kepler photometry of the prototypical Blazhko star RR Lyr: an old friend seen in a new light |
| AU : | KOLENBERG (K.); BRYSON (S.); SZABO (R.); KURTZ (D. W.); SMOLEC (R.); NEMEC (J. M.); GUGGENBERGER (E.); MOSKALIK (P.); BENKÖ (J. M.); CHADID (M.); JEON (Y.-B.); KISS (L. L.); KOPACKI (G.); NUSPL (J.); STILL (M.); CHRISTENSEN-DALSGAARD (J.); KJELDSEN (H.); BORUCKI (W. J.); CALDWELL (D. A.); JENKINS (J. M.); KOCH (D.) |
| AF : | Institut für Astronomie, University of Vienna, Türkenschanzstrasse 17/1180 Vienna/Autriche (1 aut., 5 aut., 7 aut.); NASA Ames Research Center, MS 244-30/Moffet Field, CA 94035/Etats-Unis (2 aut., 15 aut., 18 aut., 21 aut.); Konkoly Observatory of the Hungarian Academy of Sciences, Quarter Thege Miklós út 15-17/1121 Budapest/Hongrie (3 aut., 9 aut., 12 aut., 14 aut.); Jeremiah Horrocks Institute of Astrophysics, University of Central Lancashire/Preston PR1 2HE/Royaume-Uni (4 aut.); Department of Physics & Astronomy, Camosun College/Victoria, British Columbia, V8P 5J2/Canada (6 aut.); Copernicus Astronomical Center, ul. Bartycka 18/00-716 Warsaw/Pologne (8 aut.); Observatoire de la Côte dAzur, Université Nice Sophia-Antipolis, UMR 6525, Parc Valrose/06108 Nice/France (10 aut.); Korea Astronomy and Space Science Institute/Daejeon 305-348/Corée, République de (11 aut.); Sydney Insitute for Astronomy, School of Physics, University of Sydney/NSW 2006/Australie (12 aut.); Instytut Astronomiczny Uniwersytetu Wroclawskiego, Kopernika 11/51-622 Wroclaw/Pologne (13 aut.); Department of Physics and Astronomy, Aarhus University/8000 Aarhus/Danemark (16 aut., 17 aut.); SETI Institute/Mountain View, CA 94043/Etats-Unis (19 aut., 20 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 411; No. 2; Pp. 878-890; Bibl. 1/2 p. |
| LA : | Anglais |
| EA : | We present our analysis of the long-cadence Kepler data for the well-studied Blazhko star RR Lyr, gathered during the first two quarters of the satellite's observations and covering a total of 127 d. Besides being of great importance for our understanding of RR Lyrae stars in general, these RR Lyr data can be regarded as a case study for observations of bright stars with Kepler. Kepler can perform high-precision photometry on targets like RR Lyr, as the saturated flux is conserved to a very high degree. The Kepler data on RR Lyr are revolutionary in several respects. Even with long-cadence sampling (one measurement per 29.4 min), the unprecedented precision (< mmag) of the Kepler photometry allows the study of the star's extreme light-curve variations in detail. The multiplet structures at the main frequency and its harmonics, typical for Blazhko stars, are clearly detected up to the quintuplets. For the first time, photometric data of RR Lyr reveal the presence of half-integer frequencies, linked to a period-doubling effect. This phenomenon may be connected to the still unexplained Blazhko modulation. Moreover, with three observed Blazhko cycles at our disposal, we observe that there is no exact repetition in the light-curve changes from one modulation cycle to the next for RR Lyr. This may be due to additional periodicities in the star, or to transient or quasi-periodic changes. |
| CC : | 001E03 |
| FD : | Photométrie; Observation par satellite; Etoile type RR Lyrae; Etude cas; Etoile brillante; Lumière stellaire; Etoile S; Courbe lumière; Multiplet; Périodicité; Etoile branche horizontale |
| ED : | Photometry; Satellite observation; RR Lyrae stars; Case study; Bright star; Star light; S stars; Light curves; Multiplets; Periodicity; Horizontal-branch stars |
| SD : | Observación por satélite; Estudio caso; Estrella brillante; Luz estelar; Periodicidad |
| LO : | INIST-2067.354000194391580110 |
| ID : | 11-0114653 |
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Guggenberger</name><affiliation><inist:fA14 i1="01"><s1>Institut für Astronomie, University of Vienna, Türkenschanzstrasse 17</s1><s2>1180 Vienna</s2><s3>AUT</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Moskalik, P" sort="Moskalik, P" uniqKey="Moskalik P" first="P." last="Moskalik">P. Moskalik</name><affiliation><inist:fA14 i1="06"><s1>Copernicus Astronomical Center, ul. Bartycka 18</s1><s2>00-716 Warsaw</s2><s3>POL</s3><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Benko, J M" sort="Benko, J M" uniqKey="Benko J" first="J. M." last="Benkö">J. M. 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Kiss</name><affiliation><inist:fA14 i1="03"><s1>Konkoly Observatory of the Hungarian Academy of Sciences, Quarter Thege Miklós út 15-17</s1><s2>1121 Budapest</s2><s3>HUN</s3><sZ>3 aut.</sZ><sZ>9 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="09"><s1>Sydney Insitute for Astronomy, School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kopacki, G" sort="Kopacki, G" uniqKey="Kopacki G" first="G." last="Kopacki">G. Kopacki</name><affiliation><inist:fA14 i1="10"><s1>Instytut Astronomiczny Uniwersytetu Wroclawskiego, Kopernika 11</s1><s2>51-622 Wroclaw</s2><s3>POL</s3><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Nuspl, J" sort="Nuspl, J" uniqKey="Nuspl J" first="J." last="Nuspl">J. Nuspl</name><affiliation><inist:fA14 i1="03"><s1>Konkoly Observatory of the Hungarian Academy of Sciences, Quarter Thege Miklós út 15-17</s1><s2>1121 Budapest</s2><s3>HUN</s3><sZ>3 aut.</sZ><sZ>9 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Still, M" sort="Still, M" uniqKey="Still M" first="M." last="Still">M. Still</name><affiliation><inist:fA14 i1="02"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Christensen Dalsgaard, J" sort="Christensen Dalsgaard, J" uniqKey="Christensen Dalsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name><affiliation><inist:fA14 i1="11"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation><inist:fA14 i1="11"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Borucki, W J" sort="Borucki, W J" uniqKey="Borucki W" first="W. J." last="Borucki">W. J. Borucki</name><affiliation><inist:fA14 i1="02"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Caldwell, D A" sort="Caldwell, D A" uniqKey="Caldwell D" first="D. A." last="Caldwell">D. A. Caldwell</name><affiliation><inist:fA14 i1="12"><s1>SETI Institute</s1><s2>Mountain View, CA 94043</s2><s3>USA</s3><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jenkins, J M" sort="Jenkins, J M" uniqKey="Jenkins J" first="J. M." last="Jenkins">J. M. Jenkins</name><affiliation><inist:fA14 i1="12"><s1>SETI Institute</s1><s2>Mountain View, CA 94043</s2><s3>USA</s3><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Koch, D" sort="Koch, D" uniqKey="Koch D" first="D." last="Koch">D. Koch</name><affiliation><inist:fA14 i1="02"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0114653</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0114653 INIST</idno><idno type="RBID">Pascal:11-0114653</idno><idno type="wicri:Area/PascalFrancis/Corpus">001F91</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Kepler photometry of the prototypical Blazhko star RR Lyr: an old friend seen in a new light</title><author><name sortKey="Kolenberg, K" sort="Kolenberg, K" uniqKey="Kolenberg K" first="K." last="Kolenberg">K. Kolenberg</name><affiliation><inist:fA14 i1="01"><s1>Institut für Astronomie, University of Vienna, Türkenschanzstrasse 17</s1><s2>1180 Vienna</s2><s3>AUT</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bryson, S" sort="Bryson, S" uniqKey="Bryson S" first="S." last="Bryson">S. Bryson</name><affiliation><inist:fA14 i1="02"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Szabo, R" sort="Szabo, R" uniqKey="Szabo R" first="R." last="Szabo">R. Szabo</name><affiliation><inist:fA14 i1="03"><s1>Konkoly Observatory of the Hungarian Academy of Sciences, Quarter Thege Miklós út 15-17</s1><s2>1121 Budapest</s2><s3>HUN</s3><sZ>3 aut.</sZ><sZ>9 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kurtz, D W" sort="Kurtz, D W" uniqKey="Kurtz D" first="D. W." last="Kurtz">D. W. Kurtz</name><affiliation><inist:fA14 i1="04"><s1>Jeremiah Horrocks Institute of Astrophysics, University of Central Lancashire</s1><s2>Preston PR1 2HE</s2><s3>GBR</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Smolec, R" sort="Smolec, R" uniqKey="Smolec R" first="R." last="Smolec">R. Smolec</name><affiliation><inist:fA14 i1="01"><s1>Institut für Astronomie, University of Vienna, Türkenschanzstrasse 17</s1><s2>1180 Vienna</s2><s3>AUT</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Nemec, J M" sort="Nemec, J M" uniqKey="Nemec J" first="J. M." last="Nemec">J. M. Nemec</name><affiliation><inist:fA14 i1="05"><s1>Department of Physics & Astronomy, Camosun College</s1><s2>Victoria, British Columbia, V8P 5J2</s2><s3>CAN</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Guggenberger, E" sort="Guggenberger, E" uniqKey="Guggenberger E" first="E." last="Guggenberger">E. Guggenberger</name><affiliation><inist:fA14 i1="01"><s1>Institut für Astronomie, University of Vienna, Türkenschanzstrasse 17</s1><s2>1180 Vienna</s2><s3>AUT</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Moskalik, P" sort="Moskalik, P" uniqKey="Moskalik P" first="P." last="Moskalik">P. Moskalik</name><affiliation><inist:fA14 i1="06"><s1>Copernicus Astronomical Center, ul. Bartycka 18</s1><s2>00-716 Warsaw</s2><s3>POL</s3><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Benko, J M" sort="Benko, J M" uniqKey="Benko J" first="J. M." last="Benkö">J. M. Benkö</name><affiliation><inist:fA14 i1="03"><s1>Konkoly Observatory of the Hungarian Academy of Sciences, Quarter Thege Miklós út 15-17</s1><s2>1121 Budapest</s2><s3>HUN</s3><sZ>3 aut.</sZ><sZ>9 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Chadid, M" sort="Chadid, M" uniqKey="Chadid M" first="M." last="Chadid">M. Chadid</name><affiliation><inist:fA14 i1="07"><s1>Observatoire de la Côte dAzur, Université Nice Sophia-Antipolis, UMR 6525, Parc Valrose</s1><s2>06108 Nice</s2><s3>FRA</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jeon, Y B" sort="Jeon, Y B" uniqKey="Jeon Y" first="Y.-B." last="Jeon">Y.-B. Jeon</name><affiliation><inist:fA14 i1="08"><s1>Korea Astronomy and Space Science Institute</s1><s2>Daejeon 305-348</s2><s3>KOR</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kiss, L L" sort="Kiss, L L" uniqKey="Kiss L" first="L. L." last="Kiss">L. L. Kiss</name><affiliation><inist:fA14 i1="03"><s1>Konkoly Observatory of the Hungarian Academy of Sciences, Quarter Thege Miklós út 15-17</s1><s2>1121 Budapest</s2><s3>HUN</s3><sZ>3 aut.</sZ><sZ>9 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="09"><s1>Sydney Insitute for Astronomy, School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kopacki, G" sort="Kopacki, G" uniqKey="Kopacki G" first="G." last="Kopacki">G. Kopacki</name><affiliation><inist:fA14 i1="10"><s1>Instytut Astronomiczny Uniwersytetu Wroclawskiego, Kopernika 11</s1><s2>51-622 Wroclaw</s2><s3>POL</s3><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Nuspl, J" sort="Nuspl, J" uniqKey="Nuspl J" first="J." last="Nuspl">J. Nuspl</name><affiliation><inist:fA14 i1="03"><s1>Konkoly Observatory of the Hungarian Academy of Sciences, Quarter Thege Miklós út 15-17</s1><s2>1121 Budapest</s2><s3>HUN</s3><sZ>3 aut.</sZ><sZ>9 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Still, M" sort="Still, M" uniqKey="Still M" first="M." last="Still">M. Still</name><affiliation><inist:fA14 i1="02"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Christensen Dalsgaard, J" sort="Christensen Dalsgaard, J" uniqKey="Christensen Dalsgaard J" first="J." last="Christensen-Dalsgaard">J. Christensen-Dalsgaard</name><affiliation><inist:fA14 i1="11"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kjeldsen, H" sort="Kjeldsen, H" uniqKey="Kjeldsen H" first="H." last="Kjeldsen">H. Kjeldsen</name><affiliation><inist:fA14 i1="11"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Borucki, W J" sort="Borucki, W J" uniqKey="Borucki W" first="W. J." last="Borucki">W. J. Borucki</name><affiliation><inist:fA14 i1="02"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Caldwell, D A" sort="Caldwell, D A" uniqKey="Caldwell D" first="D. A." last="Caldwell">D. A. Caldwell</name><affiliation><inist:fA14 i1="12"><s1>SETI Institute</s1><s2>Mountain View, CA 94043</s2><s3>USA</s3><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jenkins, J M" sort="Jenkins, J M" uniqKey="Jenkins J" first="J. M." last="Jenkins">J. M. Jenkins</name><affiliation><inist:fA14 i1="12"><s1>SETI Institute</s1><s2>Mountain View, CA 94043</s2><s3>USA</s3><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Koch, D" sort="Koch, D" uniqKey="Koch D" first="D." last="Koch">D. Koch</name><affiliation><inist:fA14 i1="02"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Bright star</term><term>Case study</term><term>Horizontal-branch stars</term><term>Light curves</term><term>Multiplets</term><term>Periodicity</term><term>Photometry</term><term>RR Lyrae stars</term><term>S stars</term><term>Satellite observation</term><term>Star light</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Photométrie</term><term>Observation par satellite</term><term>Etoile type RR Lyrae</term><term>Etude cas</term><term>Etoile brillante</term><term>Lumière stellaire</term><term>Etoile S</term><term>Courbe lumière</term><term>Multiplet</term><term>Périodicité</term><term>Etoile branche horizontale</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present our analysis of the long-cadence Kepler data for the well-studied Blazhko star RR Lyr, gathered during the first two quarters of the satellite's observations and covering a total of 127 d. Besides being of great importance for our understanding of RR Lyrae stars in general, these RR Lyr data can be regarded as a case study for observations of bright stars with Kepler. Kepler can perform high-precision photometry on targets like RR Lyr, as the saturated flux is conserved to a very high degree. The Kepler data on RR Lyr are revolutionary in several respects. Even with long-cadence sampling (one measurement per 29.4 min), the unprecedented precision (< mmag) of the Kepler photometry allows the study of the star's extreme light-curve variations in detail. The multiplet structures at the main frequency and its harmonics, typical for Blazhko stars, are clearly detected up to the quintuplets. For the first time, photometric data of RR Lyr reveal the presence of half-integer frequencies, linked to a period-doubling effect. This phenomenon may be connected to the still unexplained Blazhko modulation. Moreover, with three observed Blazhko cycles at our disposal, we observe that there is no exact repetition in the light-curve changes from one modulation cycle to the next for RR Lyr. This may be due to additional periodicities in the star, or to transient or quasi-periodic changes.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>411</s2></fA05><fA06><s2>2</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Kepler photometry of the prototypical Blazhko star RR Lyr: an old friend seen in a new light</s1></fA08><fA11 i1="01" i2="1"><s1>KOLENBERG (K.)</s1></fA11><fA11 i1="02" i2="1"><s1>BRYSON (S.)</s1></fA11><fA11 i1="03" i2="1"><s1>SZABO (R.)</s1></fA11><fA11 i1="04" i2="1"><s1>KURTZ (D. W.)</s1></fA11><fA11 i1="05" i2="1"><s1>SMOLEC (R.)</s1></fA11><fA11 i1="06" i2="1"><s1>NEMEC (J. M.)</s1></fA11><fA11 i1="07" i2="1"><s1>GUGGENBERGER (E.)</s1></fA11><fA11 i1="08" i2="1"><s1>MOSKALIK (P.)</s1></fA11><fA11 i1="09" i2="1"><s1>BENKÖ (J. M.)</s1></fA11><fA11 i1="10" i2="1"><s1>CHADID (M.)</s1></fA11><fA11 i1="11" i2="1"><s1>JEON (Y.-B.)</s1></fA11><fA11 i1="12" i2="1"><s1>KISS (L. L.)</s1></fA11><fA11 i1="13" i2="1"><s1>KOPACKI (G.)</s1></fA11><fA11 i1="14" i2="1"><s1>NUSPL (J.)</s1></fA11><fA11 i1="15" i2="1"><s1>STILL (M.)</s1></fA11><fA11 i1="16" i2="1"><s1>CHRISTENSEN-DALSGAARD (J.)</s1></fA11><fA11 i1="17" i2="1"><s1>KJELDSEN (H.)</s1></fA11><fA11 i1="18" i2="1"><s1>BORUCKI (W. J.)</s1></fA11><fA11 i1="19" i2="1"><s1>CALDWELL (D. A.)</s1></fA11><fA11 i1="20" i2="1"><s1>JENKINS (J. M.)</s1></fA11><fA11 i1="21" i2="1"><s1>KOCH (D.)</s1></fA11><fA14 i1="01"><s1>Institut für Astronomie, University of Vienna, Türkenschanzstrasse 17</s1><s2>1180 Vienna</s2><s3>AUT</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>7 aut.</sZ></fA14><fA14 i1="02"><s1>NASA Ames Research Center, MS 244-30</s1><s2>Moffet Field, CA 94035</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>21 aut.</sZ></fA14><fA14 i1="03"><s1>Konkoly Observatory of the Hungarian Academy of Sciences, Quarter Thege Miklós út 15-17</s1><s2>1121 Budapest</s2><s3>HUN</s3><sZ>3 aut.</sZ><sZ>9 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ></fA14><fA14 i1="04"><s1>Jeremiah Horrocks Institute of Astrophysics, University of Central Lancashire</s1><s2>Preston PR1 2HE</s2><s3>GBR</s3><sZ>4 aut.</sZ></fA14><fA14 i1="05"><s1>Department of Physics & Astronomy, Camosun College</s1><s2>Victoria, British Columbia, V8P 5J2</s2><s3>CAN</s3><sZ>6 aut.</sZ></fA14><fA14 i1="06"><s1>Copernicus Astronomical Center, ul. Bartycka 18</s1><s2>00-716 Warsaw</s2><s3>POL</s3><sZ>8 aut.</sZ></fA14><fA14 i1="07"><s1>Observatoire de la Côte dAzur, Université Nice Sophia-Antipolis, UMR 6525, Parc Valrose</s1><s2>06108 Nice</s2><s3>FRA</s3><sZ>10 aut.</sZ></fA14><fA14 i1="08"><s1>Korea Astronomy and Space Science Institute</s1><s2>Daejeon 305-348</s2><s3>KOR</s3><sZ>11 aut.</sZ></fA14><fA14 i1="09"><s1>Sydney Insitute for Astronomy, School of Physics, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>12 aut.</sZ></fA14><fA14 i1="10"><s1>Instytut Astronomiczny Uniwersytetu Wroclawskiego, Kopernika 11</s1><s2>51-622 Wroclaw</s2><s3>POL</s3><sZ>13 aut.</sZ></fA14><fA14 i1="11"><s1>Department of Physics and Astronomy, Aarhus University</s1><s2>8000 Aarhus</s2><s3>DNK</s3><sZ>16 aut.</sZ><sZ>17 aut.</sZ></fA14><fA14 i1="12"><s1>SETI Institute</s1><s2>Mountain View, CA 94043</s2><s3>USA</s3><sZ>19 aut.</sZ><sZ>20 aut.</sZ></fA14><fA20><s1>878-890</s1></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000194391580110</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/2 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0114653</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>USA</s0></fA66><fC01 i1="01" l="ENG"><s0>We present our analysis of the long-cadence Kepler data for the well-studied Blazhko star RR Lyr, gathered during the first two quarters of the satellite's observations and covering a total of 127 d. Besides being of great importance for our understanding of RR Lyrae stars in general, these RR Lyr data can be regarded as a case study for observations of bright stars with Kepler. Kepler can perform high-precision photometry on targets like RR Lyr, as the saturated flux is conserved to a very high degree. The Kepler data on RR Lyr are revolutionary in several respects. Even with long-cadence sampling (one measurement per 29.4 min), the unprecedented precision (< mmag) of the Kepler photometry allows the study of the star's extreme light-curve variations in detail. The multiplet structures at the main frequency and its harmonics, typical for Blazhko stars, are clearly detected up to the quintuplets. For the first time, photometric data of RR Lyr reveal the presence of half-integer frequencies, linked to a period-doubling effect. This phenomenon may be connected to the still unexplained Blazhko modulation. Moreover, with three observed Blazhko cycles at our disposal, we observe that there is no exact repetition in the light-curve changes from one modulation cycle to the next for RR Lyr. This may be due to additional periodicities in the star, or to transient or quasi-periodic changes.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Photométrie</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Photometry</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Observation par satellite</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Satellite observation</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Observación por satélite</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Etoile type RR Lyrae</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>RR Lyrae stars</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Etude cas</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Case study</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Estudio caso</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Etoile brillante</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Bright star</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Estrella brillante</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Lumière stellaire</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Star light</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Luz estelar</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Etoile S</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>S stars</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Courbe lumière</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Light curves</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Multiplet</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Multiplets</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Périodicité</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Periodicity</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Periodicidad</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Etoile branche horizontale</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Horizontal-branch stars</s0><s5>36</s5></fC03><fN21><s1>073</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 11-0114653 INIST</NO><ET>Kepler photometry of the prototypical Blazhko star RR Lyr: an old friend seen in a new light</ET><AU>KOLENBERG (K.); BRYSON (S.); SZABO (R.); KURTZ (D. W.); SMOLEC (R.); NEMEC (J. M.); GUGGENBERGER (E.); MOSKALIK (P.); BENKÖ (J. M.); CHADID (M.); JEON (Y.-B.); KISS (L. L.); KOPACKI (G.); NUSPL (J.); STILL (M.); CHRISTENSEN-DALSGAARD (J.); KJELDSEN (H.); BORUCKI (W. J.); CALDWELL (D. A.); JENKINS (J. M.); KOCH (D.)</AU><AF>Institut für Astronomie, University of Vienna, Türkenschanzstrasse 17/1180 Vienna/Autriche (1 aut., 5 aut., 7 aut.); NASA Ames Research Center, MS 244-30/Moffet Field, CA 94035/Etats-Unis (2 aut., 15 aut., 18 aut., 21 aut.); Konkoly Observatory of the Hungarian Academy of Sciences, Quarter Thege Miklós út 15-17/1121 Budapest/Hongrie (3 aut., 9 aut., 12 aut., 14 aut.); Jeremiah Horrocks Institute of Astrophysics, University of Central Lancashire/Preston PR1 2HE/Royaume-Uni (4 aut.); Department of Physics & Astronomy, Camosun College/Victoria, British Columbia, V8P 5J2/Canada (6 aut.); Copernicus Astronomical Center, ul. Bartycka 18/00-716 Warsaw/Pologne (8 aut.); Observatoire de la Côte dAzur, Université Nice Sophia-Antipolis, UMR 6525, Parc Valrose/06108 Nice/France (10 aut.); Korea Astronomy and Space Science Institute/Daejeon 305-348/Corée, République de (11 aut.); Sydney Insitute for Astronomy, School of Physics, University of Sydney/NSW 2006/Australie (12 aut.); Instytut Astronomiczny Uniwersytetu Wroclawskiego, Kopernika 11/51-622 Wroclaw/Pologne (13 aut.); Department of Physics and Astronomy, Aarhus University/8000 Aarhus/Danemark (16 aut., 17 aut.); SETI Institute/Mountain View, CA 94043/Etats-Unis (19 aut., 20 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 411; No. 2; Pp. 878-890; Bibl. 1/2 p.</SO><LA>Anglais</LA><EA>We present our analysis of the long-cadence Kepler data for the well-studied Blazhko star RR Lyr, gathered during the first two quarters of the satellite's observations and covering a total of 127 d. Besides being of great importance for our understanding of RR Lyrae stars in general, these RR Lyr data can be regarded as a case study for observations of bright stars with Kepler. Kepler can perform high-precision photometry on targets like RR Lyr, as the saturated flux is conserved to a very high degree. The Kepler data on RR Lyr are revolutionary in several respects. Even with long-cadence sampling (one measurement per 29.4 min), the unprecedented precision (< mmag) of the Kepler photometry allows the study of the star's extreme light-curve variations in detail. The multiplet structures at the main frequency and its harmonics, typical for Blazhko stars, are clearly detected up to the quintuplets. For the first time, photometric data of RR Lyr reveal the presence of half-integer frequencies, linked to a period-doubling effect. This phenomenon may be connected to the still unexplained Blazhko modulation. Moreover, with three observed Blazhko cycles at our disposal, we observe that there is no exact repetition in the light-curve changes from one modulation cycle to the next for RR Lyr. This may be due to additional periodicities in the star, or to transient or quasi-periodic changes.</EA><CC>001E03</CC><FD>Photométrie; Observation par satellite; Etoile type RR Lyrae; Etude cas; Etoile brillante; Lumière stellaire; Etoile S; Courbe lumière; Multiplet; Périodicité; Etoile branche horizontale</FD><ED>Photometry; Satellite observation; RR Lyrae stars; Case study; Bright star; Star light; S stars; Light curves; Multiplets; Periodicity; Horizontal-branch stars</ED><SD>Observación por satélite; Estudio caso; Estrella brillante; Luz estelar; Periodicidad</SD><LO>INIST-2067.354000194391580110</LO><ID>11-0114653</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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