DOCSLIB.ORG

Chris Watkins* & James Y-K. Cho 1. Introduction 2. Gravity Waves 3. the Taylor-Goldstein Equation 4. HD 209458 B 5. Effect O

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Chris Watkins* & James Y-K. Cho 1. Introduction 2. Gravity Waves 3. the Taylor-Goldstein Equation 4. HD 209458 B 5. Effect O Gravity Wave Dynamics in Hot Extrasolar Planet Atmospheres Chris Watkins* & James Y-K. Cho Astronomy Unit, School of Mathematical Sciences, Queen Mary, University of London, Mile End Road, London, E1 4NS, UK. email: [email protected], [email protected] 1. Introduction 5. Effect on the Background Stably-stratified atmospheres can support internal gravity waves, which arise from the buoyancy of the fluid. As can be seen in Fig. 3 the wave propagates in a sheared Acceleration(ms−1 rotation−1) The waves are readily excited by heating and flow over topography and are a ubiquitous feature of the terrestrial c − u −300 −200 −100 0 100 200 300 environment. So, 0 = 0 is possible in some layer 7 −3 atmosphere. They have been intensely studied over the past several decades. They transport momentum and known as a critical layer. A wave encountering a crit- 10 heat within a fluid and the effects they have on the mean flow are routinely parametrized in GCMs of the ical layer is shown in Fig. 4. The wave is attenuated Earth’s atmosphere. by the encounter and the momentum it transports is de- 6 There are over 400 known extrasolar plan- c−u posited, causing the flow speed to change. In this case 0 ets. Their orbits and masses vary far more −1 Exoplanet Distribution the acceleration, ∼250 m s per rotation, is enough to 5 du /dt 0 1 than for the planets in the Solar System, −2 ) u 10 < 0.03 M p J double the flow speed at this layer in about 2 planetary 0.9 0.03 M − 0.25 M as shown in Fig. 1. Many planets are very J J rotations. In reality a spectrum of waves will encounter 0.25 M − 13 M 4 0.8 J J close to their parent star: nearly 70 have > 13 M critical layers over a range of altitudes, causing accel- J orbits of four days or less, they are as- 0.7 Solar System erations over the range. Thus the critical layers filter HD 209458 b 0.6 sumed to be spin-orbit synchronised. They 3 out waves, preventing them from propagating to high Pressure (bar) are exposed to a very large energy flux. 0.5 Height above 1 bar (H −1 altitudes. 10 Eccentricity w 0.4 There is much interest in modelling the 2 0.3 atmospheric circulations in these extreme Mercury −1 0.2 conditions (e.g., Cho, 2008; Showman et Heating Rate (K rotation ) −100 −50 0 50 100 1 0.1 Mars al., 2009). We consider the effects gravity 15 HD 209458 b Earth Venus −6 0 waves have on these planets by studying 14 10 0 100 200 300 400 500 600 700 800 900 1000 0 Period (days) 0 10 their behaviour in an atmosphere based on 13 −100 −50 0 50 100 Velocity (m s−1) 12 T Fig. 1: Known extrasolar planets. Solar System bodies the hot-Jupiter planet HD 209458 b. −5 Student Version of MATLAB 10 are shown for comparison and the hot-Jupiter 11 Fig. 4: A wave with c =600 m s−1 and dT /dt HD 209458 b is highlighted. (Data from exoplanet.eu) 10 0 ) p −4 2π=k =2500 km saturates in an encounter with 10 9 a critical layer near 5 Hp. 8 −3 2. Gravity Waves 7 10 6 Pressure (bar) Internal gravity waves have large scale effects in the terrestrial atmosphere - for example, the Quasi-Biennial Height above 1 bar (H 5 −2 Oscillation (Baldwin et al., 2001). They have also been observed in many Solar Systems atmospheres beyond 10 Gravity waves saturate when the temperature perturba- the Earth (e.g., Young et al., 1997). The atmospheres of extrasolar planets are expected to be stably stratified: 4 tions cause the atmosphere to become locally connec- 3 so, gravity waves will be important for modelling their dynamics. −1 tively unstable and the wave stops growing. This is 10 2 shown in Fig. 5. Here we show the heating the wave 1 induces on the background, roughly 75 K per rotation. 0 0 10 −50 0 50 Such heating could trigger new gravity waves and will 3. The Taylor-Goldstein Equation Temperature Perturbation (K) induce additional dynamical effects. Waves originat- Student Version of MATLAB The behaviour of a linear gravity wave is described by the Taylor-Goldstein equation which describes how the ing from deeper levels in the atmosphere have larger ef- −1 vertical velocity w~ varies with altitude: Fig. 5: A wave with c = −40 m s and fects. For example, excitation at the 30 bar level leads 2π=k = 2500 km saturates above 10 H . " # p to heating of nearly 3000 K per rotation. d2w^ N2 u00 u0 1 κ Q_ 0 0 2 −z=2Hρ 2 + 2 + + − 2 − k w^ = 2 e ; dz (c − u0) (c − u0) Hρ (c − u0) 4Hρ Hp (c − u0) Z z 6. Horizontal Transport −χ(z) dξ w^(z) = w~ e ; χ(z) = : For shorter waves it is possible for k2 to dominate the Index of Refraction (× 10−6 m−1) zb 2Hρ(ξ) index of refraction, which becomes imaginary (indicat- 0 10 20 30 40 50 60 15 Here c is the horizontal phase speed and k is the horizontal wavenumber. The mean flow is u0, primes are ing that the wave is evanescent). A wave is reflected _ 14 −6 differentiation w.r.t. z, and Q is the heating. In the square brackets is the index of refraction. at a layer where it becomes evanescent, as can be seen 10 13 The equation is solved numerically using Gaussian elimination with 3000 to 10000 equally spaced levels. in Fig. 6; the vertical group velocity vanishes at around 12 −5 As the equation is linear the wave can grow without bounds. To counter this a scheme is used to introduce the 10 Hp level, where Re(m) vanishes. Where there 10 11 saturation when the wave becomes convectively unstable. are layers that support propagation between evanescent 10 ) layers, the wave is ducted and energy is transported hor- p −4 izontally. The wave in Fig. 6 is an example of this. 9 10 Waves are often ducted in jets and the energy is trans- 8 −3 4. HD 209458 b ported at roughly the speed of the jet. 7 10 w The extrasolar planet HD 209458 b, is a hot-Jupiter planet that orbits its star at just 0.47 AU with a period of 6 g Pressure (bar) Re(m) u 3.52 days. It is expected to be tidally locked to its star. It has a radius of 1.32 R . Height above 1 bar (H g J 5 −2 10 −1 −1 4 Specific Gas Constant R 3523 J kg K Index of Refraction (× 10−6 m−1) 3 −1 −1 0 20 40 60 80 100 −1 Specific Heat at Constant Pressure cp 12300 J kg K 15 10 −2 2 g −6 Acceleration Due to Gravity 10 m s 14 10 Ω ×10−5 −1 1 Rotation Rate 2.08 s 13 0 0 10 0 100 200 300 400 500 600 12 −5 −1 10 Velocity (m s ) HD 2094568 b is a widely studied planet and Student Version of MATLAB 11 HD 209458b Model Zonal Flow and Temperature it is assumed to be typical for the purpose of 1520 −1 90 10 c = ) Fig. 6: A wave with 700 m s and our study. The physical parameters we used p −4 1500 9 10 2π=k = 1410 km. The vertical and horizontal are given in the table above. 60 1480 8 Re(m) group velocities and the real part of the index 1460 path −3 of refraction are shown. The forcing in our exploration is centred at 30 7 10 1440 Our Study Pressure (bar) 1 scale height above the 1 bar level. It takes 6 0 1420 the form of a modified Gaussian that is zero Height above 1 bar (H Latitude 5 −2 10 beyond two half-widths (∼ 0.3 Hp) from the 1400 Energy can be transported across vast distances in ducts −30 4 forcing centre. The heating rate we use is 1380 as Fig. 7 shows. With just one reflection the wave is car- 3 −1 modest at roughly 300 K per rotation (i.e. −60 1360 10 ried about two planetary radii across the surface. This 2 _ −3 −1 Q=cp = 10 K s ). 1340 will enable energy to be carried across the terminator 1 −90 −180 −150 −120 −90 −60 −30 0 30 60 90 120 150 180 from the day-side to the night-side. The properties of 0 Longitude 0 10 0 0.2 0.4 0.6 0.8 1 the jet will change around the planet. In places it will Distance (R ) Fig. 2: Modelled flow and temperature on HD 209458 b p become leaky and the wave will escape, via this mech- Temperature (K) Student Version of MATLAB 1300 1320 1340 1360 1380 1400 H 15 at about 1 p above the 1 bar level. The longest zonal anism heat and momentum can be transported between flow vectors are 533 m s−1. The sub-stellar point is at the Fig. 7: The path of propagation of the wave in hemispheres thus contributing to the homogenisation of 14 −6 10 centre (0◦ N, 0◦ E). Fig. 6. the atmospheric temperature. 13 12 u 0 −5 10 11 The model atmosphere used is based on simulations 10 generously shared by Thrastarson & Cho (2009), part ) p −4 7.
Load more

Recommended publications
  • Arxiv:2009.06280V1 [Astro-Ph.EP] 14 Sep 2020
    Astronomy & Astrophysics manuscript no. vis_hd20_hd18 c ESO 2020 September 15, 2020 Discriminating between hazy and clear hot-Jupiter atmospheres with CARMENES A. Sánchez-López1, M. López-Puertas2, I. A. G. Snellen1, E. Nagel3, F. F. Bauer2, E. Pallé4; 5, L. Tal-Or6; 9, P. J. Amado2, J. A. Caballero7, S. Czesla8, L. Nortmann9, A. Reiners9, I. Ribas10; 11, A. Quirrenbach12, J. Aceituno13, V. J. S. Béjar4; 5, N. Casasayas-Barris4; 5, Th. Henning14, K. Molaverdikhani14, D. Montes15, M. Stangret4; 5, M. R. Zapatero Osorio16, and M. Zechmeister9 1 Leiden Observatory, Leiden University, Postbus 9513, 2300 RA, Leiden, The Netherlands e-mail: [email protected] 2 Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, 18008 Granada, Spain 3 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany 4 Instituto de Astrofísica de Canarias (IAC), Calle Vía Láctea s/n, 38200 La Laguna, Tenerife, Spain 5 Departamento de Astrofísica, Universidad de La Laguna, 38026 La Laguna, Tenerife, Spain 6 Department of Physics, Ariel University, Ariel 40700, Israel 7 Centro de Astrobiología (CSIC-INTA), ESAC, Camino bajo del castillo s/n, 28692 Villanueva de la Cañada, Madrid, Spain 8 Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany 9 Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany 10 Institut de Ciències de l’Espai (CSIC-IEEC), Campus UAB, c/ de Can Magrans s/n, 08193 Bellaterra, Barcelona, Spain 11 Institut d’Estudis Espacials
    [Show full text]
  • Evidence of Energy-, Recombination-, and Photon-Limited Escape Regimes in Giant Planet H/He Atmospheres M
    A&A 648, L7 (2021) Astronomy https://doi.org/10.1051/0004-6361/202140423 & c ESO 2021 Astrophysics LETTER TO THE EDITOR Evidence of energy-, recombination-, and photon-limited escape regimes in giant planet H/He atmospheres M. Lampón1, M. López-Puertas1, S. Czesla2, A. Sánchez-López3, L. M. Lara1, M. Salz2, J. Sanz-Forcada4, K. Molaverdikhani5,6, A. Quirrenbach6, E. Pallé7,8, J. A. Caballero4, Th. Henning5, L. Nortmann9, P. J. Amado1, D. Montes10, A. Reiners9, and I. Ribas11,12 1 Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, 18008 Granada, Spain e-mail: [email protected] 2 Hamburger Sternwarte, Universität Hamburg,Gojenbergsweg 112, 21029 Hamburg, Germany 3 Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands 4 Centro de Astrobiología (CSIC-INTA), ESAC, Camino bajo del castillo s/n, 28692, Villanueva de la Cañada Madrid, Spain 5 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany 6 Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany 7 Instituto de Astrofísica de Canarias (IAC), Calle Vía Láctea s/n, 38200, La Laguna Tenerife, Spain 8 Departamento de Astrofísica, Universidad de La Laguna, 38026, La Laguna Tenerife, Spain 9 Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany 10 Departamento de Física de la Tierra y Astrofísica & IPARCOS-UCM (Instituto de Física de Partículas y del Cosmos de la UCM), Facultad de Ciencias Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain 11 Institut de Ciències de l’Espai (CSIC-IEEC), Campus UAB, c/ de Can Magrans s/n, 08193 Bellaterra, Barcelona, Spain 12 Institut d’Estudis Espacials de Catalunya (IEEC), 08034 Barcelona, Spain Received 26 January 2021 / Accepted 19 March 2021 ABSTRACT Hydrodynamic escape is the most efficient atmospheric mechanism of planetary mass loss and has a large impact on planetary evolution.
    [Show full text]
  • Atmospheric Mass Loss of Extrasolar Planets Orbiting Magnetically Active
    MNRAS 000, 1–?? (2017) Preprint 8 August 2018 Compiled using MNRAS LATEX style file v3.0 Atmospheric mass loss of extrasolar planets orbiting magnetically active host stars Lalitha Sairam,1⋆ J. H. M. M. Schmitt,2 and Spandan Dash3 1Indian Institute of Astrophysics, II Block, Koramangala, Bangalore 560 034, India 2Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg 3Indian Institute of Science, C.V Raman Avenue, Yeshwantpur, Bangalore 560 012, India Accepted XXX. Received YYY; in original form ZZZ ABSTRACT Magnetic stellar activity of exoplanet hosts can lead to the production of large amounts of high-energy emission, which irradiates extrasolar planets, located in the immediate vicinity of such stars. This radiation is absorbed in the planets’ upper atmospheres, which consequently heat up and evaporate, possibly leading to an irradiation-induced mass-loss. We present a study of the high-energy emission in the four magnetically ac- tive planet-bearing host stars Kepler-63, Kepler-210, WASP-19, and HAT-P-11, based on new XMM-Newton observations. We find that the X-ray luminosities of these stars are rather high with orders of magnitude above the level of the active Sun. The total XUV irradiation of these planets is expected to be stronger than that of well stud- ied hot Jupiters. Using the estimated XUV luminosities as the energy input to the planetary atmospheres, we obtain upper limits for the total mass loss in these hot Jupiters. Key words: stars: activity – stars: coronae – stars: low-mass, late-type, planetary systems – stars: individual: Kepler-63, Kepler-210, WASP-19, HAT-P-11 1 INTRODUCTION through Jeans escape, the observations of atmospheric mass loss in HD 209458 b (Vidal-Madjar et al.
    [Show full text]
  • Introduction
    Introduction Onething is certain about this book: by thetimeyou readit, parts of it will be out of date. Thestudy of exoplanets,planets orbitingaround starsother than theSun, is anew andfast-moving field.Important newdiscoveries areannounced on a weekly basis. This is arguablythe most exciting andfastest-growing field in astrophysics.Teamsofastronomersare competing to be thefirsttofind habitable planets likeour ownEarth, andare constantly discovering ahostofunexpected andamazingly detailed characteristics of thenew worlds. Since1995, when the first exoplanet wasdiscoveredorbitingaSun-like star,over 400 of them have been identified.Acomprehensive review of thefield of exoplanets is beyond thescope of this book, so we have chosen to focus on thesubset of exoplanets that are observedtotransittheir hoststar (Figure 1). Figure1 An artist’simpression of thetransitofHD209458 bacrossits star. Thesetransitingplanets areofparamount importancetoour understanding of the formation andevolutionofplanets.During atransit, theapparent brightness of the hoststar drops by afraction that is proportionaltothe area of theplanet: thus we can measure thesizes of transitingplanets,eventhough we cannot seethe planets themselves.Indeed,the transitingexoplanets arethe onlyplanets outside our own Solar System with known sizes.Knowing aplanet’ssize allows its density to be deduced andits bulk compositiontobeinferred.Furthermore, by performing precisespectroscopicmeasurements during andout of transit, theatmospheric compositionofthe planet can be detected.Spectroscopicmeasurements
    [Show full text]
  • Dr. Avi Mandell (NASA) “Somewhere, Something Incredible Is Waiting to Be Known.” - Carl Sagan
    The Age of Exoplanets: From First Discoveries to the Search for Living Worlds Dr. Avi Mandell (NASA) “Somewhere, something incredible is waiting to be known.” - Carl Sagan How will the discovery of a distant planet teeming with life change our perspective on our own planet – and on ourselves? Planets 101: Our Solar SysteM Planets 101: Our Solar SysteM First Planet Around a Sun-Like Star Discovered in 1995 Notable Facts About 1995: • Bill Clinton is in his 3rd year of the Presidency • Ebay opens for business •DVDs are first introduced •Big event for the coffee-drinking world… Invention of the Frappucino! The First Planets were Discovered by Measuring The Motions of Stars 51 Peg b • Uses the change in star’s light due to the Doppler effect Mayor & Queloz, Movie: eso1035g.mov November 1995 Dr. Michel Mayor & Dr. Didier Queloz Geneva Observatory Spectrum of Starlight from Dr. Geoff Marcy & Parent Star Dr. R. Paul Butler San Francisco State Univ. Timeline of Exoplanet Discoveries Known Exoplanets, 1995: 0 Planet Mass Jup. Neptune Earth Mercury Earth Jupiter Distance to the Star Timeline of Exoplanet Discoveries Known Exoplanets, 1996: 6 Planet Mass Jup. First Confirmed RV Planet: 51 Peg b Neptune Earth Mercury Earth Jupiter Distance to the Star Timeline of Exoplanet Discoveries Known Exoplanets, 1996: 6 2000: 38 Planet Mass First Transiting Planet: Jup. HD 209458 b First Confirmed RV Planet: 51 Peg b Neptune Earth Mercury Earth Jupiter Distance to the Star The Most Planets have been Discovered by Measuring The Shadows on Stars Movie: OccultationGraphH264FullSize.mov Timeline of Exoplanet Discoveries Known Exoplanets, 2000: 38 2005: 155 2008: 260 2012: 579 Planet Mass Jup.
    [Show full text]
  • A Spit.Ze@ Infrared Radius for the Transiting Extrasolar Planet HD 209458 B
    * Source of Acquisition PAGoddard Space night Center Accepted to Astrophysical Journal A Spit.ze@ Infrared Radius for the Transiting Extrasolar Planet HD 209458 b L. Jeremy Richardson Exoplanets and Stellar Astrophysics Laboratory, NASA's Goddard Space Flight Center, Mail Code 667, Greenbelt, MD 20771 [email protected] Joseph Harrington Center for Radiophysics and Space Research, Cornell Universtiy, 326 Space Sciences Bldg., Ithaca, N Y 14 853- 6801 [email protected] Sara Seager Department of Terrestrial Magnetism, Carnegie Institution of Washington, 524 1 Broad Branch Rd NW, Washington, DC 20015 [email protected] Drake Deming Planetary Systems Laboratory, NASA 's Goddard Space Flight Center, Mail Code 693, Greenbelt, MD 20771 [email protected] ABSTRACT We have measured the infrared transit of the extrasolar planet HD 209458 b using the Spitzer Space Telescope. We observed two primary eclipse events (one partial and one complete transit) using the 24 pm array of the Multiband Imaging Photometer for Spitzer (MIPS). We analyzed a total of 2392 individual images (10-second integrations) of the planetary system, recorded before, during, and after transit. We perform optimal photometry on the images and use the local -2- zodiacal light as a short-term flux reference. At this long wavelength, the tran- sit curve has a simple box-like shape, allowing robust solutions for the stellar and planetary radii independent of stellar limb darkening, which is negligible at 24 pm. We derive a stellar radius of R, = 1.06 f 0.07 b,a planetary radius of Rp = 1.26 f 0.08 RJ, and a stellar mass of 1.17 M,.
    [Show full text]
  • Atmospheres of Hot Alien Worlds
    Atmospheres of hot alien Worlds Atmospheres of hot alien Worlds Proefschrift ter verkrijging van de graad van Doctor aan de Universiteit Leiden, op gezag van Rector Magnificus prof.mr. C.J.J.M. Stolker, volgens besluit van het College voor Promoties te verdedigen op donderdag 5 juni 2014 klokke 10.00 uur door Matteo Brogi geboren te Grosseto, Italië in 1983 Promotiecommissie Promotors: Prof. dr. I. A. G. Snellen Prof. dr. C. U. Keller Overige leden: Prof. dr. C. Dominik University of Amsterdam Prof. dr. K. Heng University of Bern Prof. dr. E. F. van Dishoeck Dr. M. A. Kenworthy Prof. dr. H. J. A. Röttgering Ai miei genitori, per aver creduto in me, permettendomi di realizzare un sogno Contents 1 Introduction 1 1.1 Planet properties from transits and radial velocities . 2 1.2 Atmospheric characterization of exoplanets . 4 1.2.1 Atmospheres of transiting planets . 4 1.2.2 Challenges of space- and ground-based observations . 7 1.2.3 Ground-based, high resolution spectroscopy . 8 1.2.4 A novel data analysis . 10 1.3 Close-in planets and their environment . 10 1.3.1 From atmospheric escape to catastrophic evaporation . 12 1.4 This thesis . 12 2 The orbital trail of the giant planet t Boötis b 17 2.1 The CRIRES observations . 18 2.2 Data reduction and analysis . 19 2.2.1 Initial data reduction . 19 2.2.2 Removal of telluric line contamination . 19 2.2.3 Cross correlation and signal extraction . 21 2.3 The CO detection and the planet velocity trail .
    [Show full text]
  • Extrasolar Planets
    Extrasolar Planets Dieter Schmitt Lecture Max Planck Institute for Introduction to Solar System Research Solar System Physics KatlenburgLindau Uni Göttingen, 8 June 2009 Outline • Historical Overview • Detection Methods • Planet Statistics • Formation of Planets • Physical Properties • Habitability Historical overview • 1989: planet / brown dwarf orbiting HD 114762 (Latham et al.) • 1992: two planets orbiting pulsar PSR B1257+12 (Wolszczan & Frail) • 1995: first planet around a solarlike star 51 Peg b (Mayor & Queloz) • 1999: first multiple planetary system with three planets Ups And (Edgar et al.) • 2000: first planet by transit method HD 209458 b (Charbonneau et al.) • 2001: atmosphere of HD 209458 b (Charbonneau et al.) • 2002: astrometry applied to Gliese 876 (Benedict et al.) • 2005: first planet by direct imaging GQ Lupi b (Neuhäuser et al.) • 2006: Earthlike planet by gravitational microlensing (Beaulieu et al.) • 2007: Gliese 581d, small exoplanet near habitability zone (Selsis et al.) • 2009: Gliese 581e, smallest exoplanet with 1.9 Earth masses (Mayor et al.) • As of 7 June 2009: 349 exoplanets in 296 systems (25 systems with 2 planets, 9 with 3, 2 with 4 and 1 with 5) www.exoplanet.eu Our Solar System 1047 MJ 0.39 AU 0.00314 MJ 1 MJ 0.30 MJ 0.046 MJ 0.054 MJ 1 AU 5.2 AU 9.6 AU 19 AU 30 AU 1 yr 11.9 yr 29.5 yr 84 yr 165 yr Definition Planet IAU 2006: • in orbit around the Sun / star • nearly spherical shape / sufficient mass for hydrostatic equilib. • cleared neighbourhood around its orbit Pluto: dwarf planet, as Ceres Brown
    [Show full text]
  • FTIR Spectroscopy of Hot Exoplanets: a First Step in Experimental Procedure and Analysis
    BearWorks MSU Graduate Theses Spring 2017 FTIR Spectroscopy of Hot Exoplanets: A First Step in Experimental Procedure and Analysis Heath Emmanuel Gemar As with any intellectual project, the content and views expressed in this thesis may be considered objectionable by some readers. However, this student-scholar’s work has been judged to have academic value by the student’s thesis committee members trained in the discipline. The content and views expressed in this thesis are those of the student-scholar and are not endorsed by Missouri State University, its Graduate College, or its employees. Follow this and additional works at: https://bearworks.missouristate.edu/theses Part of the Materials Science and Engineering Commons Recommended Citation Gemar, Heath Emmanuel, "FTIR Spectroscopy of Hot Exoplanets: A First Step in Experimental Procedure and Analysis" (2017). MSU Graduate Theses. 3165. https://bearworks.missouristate.edu/theses/3165 This article or document was made available through BearWorks, the institutional repository of Missouri State University. The work contained in it may be protected by copyright and require permission of the copyright holder for reuse or redistribution. For more information, please contact [email protected]. FTIR SPECTROSCOPY OF HOT EXOPLANETS: A FIRST STEP IN EXPERIMENTAL PROCEDURE AND ANALYSIS A Master’s Thesis Presented to The Graduate College of Missouri State University TEMPLATE In Partial Fulfillment Of the Requirements for the Degree Master of Science, Materials Science By Heath Gemar May, 2017 Copyright 2017 by Heath Emmanuel Gemar ii FTIR SPECTROSCOPY OF HOT EXOPLANETS: A FIRST STEP IN EXPERIMENTAL PROCEDURE AND ANALYSIS Physics, Astronomy, and Materials Science Missouri State University, May 2017 Master of Science Heath Gemar ABSTRACT In this thesis, I demonstrate how I constructed a complete experimental package to view FTIR Spectroscopy of constituents that make up hot, rocky exoplanets.
    [Show full text]
  • A CRIRES-Search for H3+ Emission from the Hot Jupiter Atmosphere Of
    A&A 589, A99 (2016) Astronomy DOI: 10.1051/0004-6361/201525675 & c ESO 2016 Astrophysics A CRIRES-search for H+ emission from the hot Jupiter atmosphere 3 of HD 209458 b? (Research Note) L. F. Lenz1, A. Reiners1, A. Seifahrt2, and H. U. Käufl3 1 Institute for Astrophysics, University of Goettingen, Friedrich-Hund-Platz 1, 37077 Goettingen, Germany e-mail: [email protected] 2 Department of Astronomy and Astrophysics, University of Chicago, IL 60637, USA 3 European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748 Garching, Germany Received 16 January 2015 / Accepted 11 March 2016 ABSTRACT + Close-in extrasolar giant planets are expected to cool their thermospheres by producing H3 emission in the near-infrared (NIR), but + simulations predict H3 emission intensities that differ in the resulting intensity by several orders of magnitude. We want to test the + observability of H3 emission with CRIRES at the Very Large Telescope (VLT), providing adequate spectral resolution for planetary + 0 atmospheric lines in NIR spectra. We search for signatures of planetary H3 emission in the L band, using spectra of HD 209458 + obtained during and after secondary eclipse of its transiting planet HD 209458 b. We searched for H3 emission signatures in spectra containing the combined light of the star and, possibly, the planet. With the information on the ephemeris of the transiting planet, we derive the radial velocities at the time of observation and search for the emission at the expected line positions. We also apply a cross-correlation test to search for planetary signals and use a shift and add technique combining all observed spectra taken after + secondary eclipse to calculate an upper emission limit.
    [Show full text]
  • On the Detection of Extrasolar Moons and Rings
    On the Detection of Extrasolar Moons and Rings Rene´ Heller Revised 3 August 2017 Abstract Since the discovery of a planet transiting its host star in the year 2000, thousands of additional exoplanets and exoplanet candidates have been detected, mostly by NASA’s Kepler space telescope. Some of them are almost as small as the Earth’s moon. As the solar system is teeming with moons, more than a hundred of which are in orbit around the eight local planets, and with all of the local giant planets showing complex ring systems, astronomers have naturally started to search for moons and rings around exoplanets in the past few years. We here discuss the principles of the observational methods that have been proposed to find moons and rings beyond the solar system and we review the first searches. Though no exomoon or exoring has been unequivocally validated so far, theoretical and technological requirements are now on the verge of being mature for such discoveries. Introduction – Why bother about moons? The moons of the solar system planets have become invaluable tracers of the local planet formation and bombardment, e.g. for the Earth-Moon system (Cameron and Ward 1976; Rufu et al 2017) and for Mars and its tiny moons Phobos and Deimos (Rosenblatt et al 2016). The composition of the Galilean moons constrains the tem- perature distribution in the accretion disk around Jupiter 4.5 billion years ago (Pol- lack and Reynolds 1974; Canup and Ward 2002; Heller et al 2015). And while the major moons of Saturn, Uranus, and Neptune might have formed from circumplan- etary tidal debris disks (Crida and Charnoz 2012), Neptune’s principal moon Triton has probably been caught during an encounter with a minor planet binary (Agnor and Hamilton 2006).
    [Show full text]
  • Exomoon Habitability and Tidal Evolution in Low-Mass Star Systems
    EXOMOON HABITABILITY AND TIDAL EVOLUTION IN LOW-MASS STAR SYSTEMS by Rhett R. Zollinger A dissertation submitted to the faculty of The University of Utah in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics Department of Physics and Astronomy The University of Utah December 2014 Copyright © Rhett R. Zollinger 2014 All Rights Reserved The University of Utah Graduate School STATEMENT OF DISSERTATION APPROVAL The dissertation of Rhett R. Zollinger has been approved by the following supervisory committee members: Benjamin C. Bromley Chair 07/08/2014 Date Approved John C. Armstrong Member 07/08/2014 Date Approved Bonnie K. Baxter Member 07/08/2014 Date Approved Jordan M. Gerton Member 07/08/2014 Date Approved Anil C. Seth Member 07/08/2014 Date Approved and by Carleton DeTar Chair/Dean of the Department/College/School o f _____________Physics and Astronomy and by David B. Kieda, Dean of The Graduate School. ABSTRACT Current technology and theoretical methods are allowing for the detection of sub-Earth sized extrasolar planets. In addition, the detection of massive moons orbiting extrasolar planets (“exomoons”) has become feasible and searches are currently underway. Several extrasolar planets have now been discovered in the habitable zone (HZ) of their parent star. This naturally leads to questions about the habitability of moons around planets in the HZ. Red dwarf stars present interesting targets for habitable planet detection. Compared to the Sun, red dwarfs are smaller, fainter, lower mass, and much more numerous. Due to their low luminosities, the HZ is much closer to the star than for Sun-like stars.
    [Show full text]