Suche Nach Extrasolaren Planeten Durch Beobachtung Von Transitzeitvariationen

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Suche Nach Extrasolaren Planeten Durch Beobachtung Von Transitzeitvariationen Suche nach extrasolaren Planeten durch Beobachtung von Transitzeitvariationen Dissertation zur Erlangung des akademischen Grades doctor rerum naturalium (Dr. rer. nat.) vorgelegt dem Rat der Physikalisch-Astronomischen Fakultät der Friedrich-Schiller-Universität Jena von Dipl.-Phys. Stefanie Rätz geboren am 28. 01. 1984 in Bad Salzungen Gutachter 1. Prof. Dr. Ralph Neuhäuser Friedrich-Schiller-Universität Jena Physikalisch-Astronomische Fakultät Astrophysikalisches Institut und Universitäts-Sternwarte 2. Prof. Dr. Stefan Dreizler Georg-August-Universität Göttingen Fakultät für Physik Institut für Astrophysik 3. Prof. Dr. Heike Rauer Deutsches Zentrum für Luft- und Raumfahrt (DLR) Berlin Institut für Planetenforschung Extrasolare Planeten und Atmosphären Tag der Disputation: 05.07.2012 Thesen zur Dissertation Suche nach extrasolaren Planeten durch Beobachtung von Transitzeitvariationen vorgelegt von Diplom-Physiker Stefanie Rätz ——————————————————————————————————————– 1. Homogene Beobachtung und Auswertung von Transitlichtkurven von sehr hoher Qualität kann zur Identifizierung von Transitzeitvariationen führen. Bei den boden- gebundenen Beobachtungen wurden nur Transitzeiten berücksichtigt, die in einer der an „Transit Timing Variations @ YETI” (TTV@YETI) beteiligten Sternwarten gewonnen wurden. Zusätzlich wurden Daten des NASA-Weltraumteleskops Kepler ausgewertet. 2. Starkes Defokussieren führt zu einer deutlichen Erhöhung der Qualität der Licht- kurven bei gegebenen Teleskop und Instrument. 3. Für den Transitplaneten TrES-2 wurden fünf Jahre Beobachtungen der Universitäts- Sternwarte Jena und von TTV@YETI zusammen mit sechs Beobachtungsquartalen von Kepler ausgewertet. Der lange Beobachtungszeitraum ermöglicht die sehr prä- zise Neubestimmung der Transitephemeriden. 4. Für insgesamt 210 Transits von TrES-2 wurde die Zeit des Transitmittelpunkte bestimmt. Die Transitzeiten zeigen weder Variationen auf langen noch auf kurzen Zeitskalen. 5. Die nahezu kontinuierlichen Beobachtungen von Kepler zeigen keine statistisch si- gnifikante Zu- oder Abnahme der Systemparameter. Auch die in früheren Publika- tionen prognistizierte Änderung der Inklination konnte nicht bestätigt werden. Im Rahmen der erreichten Genauigkeit kann allerdings ein leichter Anstieg auch nicht ausgeschlossen werden. 6. Die Zusammenfassung von 84 Kepler-Lichtkurven erzielt ein Signal-Rausch-Ver- hältnis von 761. Die Modellierung mit einer analytischen Lichtkurve und linearer Randverdunklung zeigt eine Abweichung von der beobachteten Lichtkurve, während das quadratische Randverdunklungsgesetz die Beobachtungen gut wiedergibt. 7. Die CCD-Kamera STK am 90/60 cm Teleskop der Universitäts-Sternwarte Jena ist durch ihr großes Gesichtsfeld ein exzellentes Gerät für die Beobachtung der Transits von WASP-14 b. 8. Zur Bestimmung der Systemparameter vom WASP-14 wurden fünf Transits zu- sammengefasst. Die Genauigkeit der Literaturwerte wurde erreicht. Anhand der Systemparameter wurden die physikalischen Eigenschaften des Systems berechnet. 9. WASP-14 b zeigt in Beobachtungen der Jahre 2009 und 2011 nach der Neubestim- mung der Ephemeriden Hinweise auf sinusförmige Transitzeitvariationen. Dieses Sig- nal konnte mit den neusten Beobachtungen Anfang 2012 nicht bestätigt werden. Inhaltsverzeichnis 1 Einleitung 1 1.1Transitmethode................................. 3 1.1.1 Geometrie................................ 3 1.1.2 Lichtkurvenform............................ 5 1.2Transitzeitvariationen.............................. 8 1.2.1 ZusätzlichePlaneten.......................... 9 1.2.2 Monde.................................. 12 1.2.3 Trojaner................................. 13 1.2.4 Lang-Zeit-Effekte............................ 14 1.3 Gezeiten und Exzentrizität . ......................... 16 1.3.1 Gebundene Rotation . ......................... 17 1.3.2 Zirkularisierung............................. 17 1.3.3 HeißeJupitermitExzentrizität.................... 18 1.3.4 MessungderExzentrizität....................... 19 2 Beobachtung und Auswertung 20 2.1Beobachtungen................................. 20 2.1.1 Universitäts-SternwarteJena...................... 21 2.1.2 TTV@YETI............................... 21 2.1.3 AuswahlderbeobachtetenTransitplaneten.............. 22 2.1.4 DefokussierteBeobachtungen..................... 25 2.2Datenreduktion................................. 27 2.3Fotometrie.................................... 28 2.3.1 Differentielle Fotometrie mit IRAF .................. 28 2.3.2 OptimaleAperturgröße......................... 29 2.3.3 DieMethodedeskünstlichenVergleichssterns............ 30 2.4Lichtkurvenanalyse............................... 30 2.4.1 Parameterkorrelationen......................... 31 2.4.2 VorgehensweisebeimFit........................ 32 2.4.3 Fehlerabschätzung........................... 33 2.5GenauigkeitderTransitbeobachtungen.................... 34 3TrES-2 36 3.1Beobachtungen................................. 38 3.2Auswertung................................... 38 3.2.1 Lichtkurvenanalyse........................... 40 3.2.2 Randverdunklung . ......................... 40 3.2.3 Beispiel: Lichtkurve vom 15. August 2009 ............... 41 i INHALTSVERZEICHNIS ii 3.2.4 Ergebnisse................................ 42 3.2.5 ZusätzlichesLichtvonschwachen,nahenObjekten.......... 45 3.3DatendesKeplerWeltraumteleskops..................... 47 3.3.1 Kepler Lichtkurvenausdem„NASAExoplanetArchive”...... 47 3.3.2 Beschreibung der verwendeten Kepler-Daten............. 48 3.3.3 Analyse der Kepler-Lichtkurven.................... 49 3.3.4 Effekt der Randverdunklung ...................... 50 3.4BestimmungderSystemparameter....................... 52 3.5ÄnderungderSystemparameter........................ 53 3.6PhysikalischenEigenschaftendesTrES-2-Systems.............. 55 3.7TransitTiming................................. 57 4WASP-14b 60 4.1Beobachtungen................................. 62 4.1.1 TTV@YETI............................... 62 4.1.2 CalarAlto................................ 64 4.2Auswertung................................... 65 4.2.1 Lichtkurvenanalyse........................... 66 4.2.2 Beispiel: Lichtkurve vom 29. März 2011 . ............... 67 4.2.3 Ergebnisse................................ 70 4.3BestimmungderSystemparameter....................... 71 4.4PhysikalischenEigenschaftendesSystems................... 73 4.5TransitTiming................................. 73 5 Zusammenfassung und Diskussion 78 A Zusätzliche Informationen 87 A.1 Einzelergebnisse aller Transits von Kepler .................. 87 A.2TransitzeitenTrES-2.............................. 92 A.3LichtkurvenvonTrES-2............................ 95 A.4LichtkurvenvonWASP-14b..........................102 Literatur 105 Danksagung 116 Lebenslauf 118 Abbildungsverzeichnis 1.1SchematischeDarstellungeinerTransitlichtkurve............... 4 1.2WinkelzwischenOberflächennormaleundSichtlinie............. 8 1.3TTVsaufgrundeineszusätzlicheninnerenPlaneten............. 10 1.4TTVsaufgrundeineszusätzlichenäußerenPlaneten............. 10 1.5 Masse des zusätzlichen Planeten als Funktion des Periodenverhältnisses . 11 1.6ZusammensetzungeinerExomond-Lichtkurve................ 12 1.7SkizzedesStern-Planet-Mond-Systems.................... 12 1.8PositionderLagrange-PunkteineinenOrbit................. 13 1.9 Schematische Darstellung der Wirkung von Gezeiten ............ 17 1.10 Die Verteilung der Exzentrizitäten als Funktion der großen Halbachse . 19 2.1 Teleskop Netzwerk TTV@YETI........................ 22 2.2VergleichvonfokussiertenunddefokussiertenBeobachtungen........ 26 2.3BestimmungderoptimalenApertur...................... 30 3.1 TrES-2 Lichtkurve vom 15. August 2009 ................... 42 3.2 Drei TrES-2 Lichtkurven vom 24.10.2010 ................... 45 3.3 TrES-2 Beobachtung vom 09.08.2011 mit CAFOS .............. 45 3.4AusschnitteinerSTKAufnahmeumTrES-2................. 46 3.5 Kepler Transit1ausQ0............................ 49 3.6 Gebinnte Lichtkurve von Kepler ........................ 50 3.7 Abbildung 3.6 gefittet mit 2 verschiedenen Modellen ............. 51 3.8ResiduenzwischenFitundModell....................... 51 3.9InklinationüberBeobachtungsepoche..................... 54 3.10HäufigkeitsverteilungfürInklination...................... 54 3.11SummedesfraktionellenRadiusüberBeobachtungsepoche......... 54 3.12HäufigkeitsverteilungfürSummedesfraktionellenRadius.......... 54 3.13RadiusverhältnisüberBeobachtungsepoche.................. 54 3.14HäufigkeitsverteilungfürRadiusverhältnis.................. 54 3.15 B − R überBeobachtungsepoche....................... 57 3.16 Häufigkeitsverteilung des B − R für Kepler .................. 57 3.17 B − R –Diagrammfüralle210ausgewertetenTransits........... 58 4.1 R-BandAufnahmevonWASP-14mitderCTK............... 63 4.2 R-BandAufnahmederSTKvonWASP-14.................. 63 4.3 V -BandCAFOS-AufnahmevonWASP-14.................. 64 4.43D-OberflächenprofilvonWASP-14mitCAFOS................ 64 4.5PartielleCAFOS-LichtkurvevonWASP-14b................. 65 4.6BesteWASP-14LichtkurvevonCAFOS................... 65 iii ABBILDUNGSVERZEICHNIS iv 4.7 WASP-14 Lichtkurve vom 29. März 2011 ................... 68 4.8 Lichtkurve von WASP-14 vom 1. April 2009 . ............... 70 4.9 Transit vom 20. März 2011 . ......................... 70 4.10GebinnteLichtkurvevonWASP-14b..................... 72 4.11 Periodogramm des B − R vonWASP14b................... 76 4.12 B − R –DiagrammfürWASP-14b...................... 76 4.13 B − R –DiagrammfürWertemithoherQualität.............. 77 4.14 B − R –DiagrammberechnetmitneuenElementen............
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