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Relevant bibliographies by topics / Star system spectroscopy / Dissertations / Theses

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Dissertations / Theses on the topic 'Star system spectroscopy'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

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1

Mukai, K. "Spectroscopic studies of AM her type systems." Thesis, University of Oxford, 1986. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.376952.

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2

Hansson, Annie. "Stark Spectroscopy, Lifetimes and Coherence Effects in Diatomic Molecular Systems." Doctoral thesis, Stockholm : Department of Physics, Stockholm University, 2005. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-650.

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3

Froning, Cynthia Suzanne. "The near-infrared properties of compact binary systems /." Digital version accessible at:, 1999. http://wwwlib.umi.com/cr/utexas/main.

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4

Blakelock, Carolyn J. "Time-resolved spectroscopy of the AM Herculis-type binary systems QQ VUL and EF ERI." Virtual Press, 1998. http://liblink.bsu.edu/uhtbin/catkey/1115429.

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Cataclysmic variable stars (CVs) are interacting binary systems. One of the stars (referred to as the primary) is a white dwarf, the other (referred to as the secondary) is usually a late main sequence star such as a red dwarf. Due to the closeness of the two stars, the white dwarf accretes gasses from the secondary. If the white dwarf does not possess a strong magnetic field, these gasses go into orbit, forming an accretion disk around the primary. If the white dwarf does possess a strong magnetic field, the gasses cannot form an accretion disk because they are entrained by the magnetic field

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5

Bruno, Giovanni. "Characterization of transiting exoplanets : analyzing the impact of the host star on the planet parameters." Thesis, Aix-Marseille, 2015. http://www.theses.fr/2015AIXM4746/document.

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Dans le cadre de ma thèse, j’ai analysé les spectres de neuf étoiles Kepler obtenus avec les relevés de vitesse radiale (VR). Cela a permis la caractérisation de leur compagnons planétaires. J’ai analysé les spectres de 21 autres étoiles CoRoT et Kepler, probablement hôtes de naines M à faible masse. Cela a permis d’'élargir l'échantillon des étoiles à faible masse avec masse et rayon mesurés. J’ai calculé l’indice d’activité chromosphérique de 31 étoiles observées avec SOPHIE/OHP, en aidant l’étude des interactions étoile-planète. J’ai étudié le comportement de SOPHIE à bas signal à bruit (S/

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6

Johnson-Groh, Mara, Christian Marois, Rosa Robert J. De, et al. "Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623816.

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We present new observations of the low-mass companion to HD 984 taken with the Gemini Planet Imager (GPI) as a part of the GPI Exoplanet Survey campaign. Images of HD 984 B were obtained in the J (1.12-1.3 mu m) and H (1.50-1.80 mu m) bands. Combined with archival epochs from 2012 and 2014, we fit the first orbit to the companion to find an 18 au (70-year) orbit with a 68% confidence interval between 14 and 28 au, an eccentricity of 0.18 with a 68% confidence interval between 0.05 and 0.47, and an inclination of 119 degrees with a 68% confidence interval between 114 degrees and 125 degrees. To

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Silverman, Lisa Nicole. "Stark spectroscopy as a probe of charge reorganization in chemical and biological systems /." May be available electronically:, 2008. http://proquest.umi.com/login?COPT=REJTPTU1MTUmSU5UPTAmVkVSPTI=&clientId=12498.

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8

Hełminiak, K. G., M. Kuzuhara, K. Mede, et al. "SEEDS DIRECT IMAGING OF THE RV-DETECTED COMPANION TO V450 ANDROMEDAE, AND CHARACTERIZATION OF THE SYSTEM." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622454.

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We report the direct imaging detection of a low-mass companion to a young, moderately active star V450. And, that was previously identified with the radial velocity (RV) method. The companion was found in high-contrast images obtained with the Subaru Telescope equipped with the HiCIAO camera and AO188 adaptive optics system. From the public ELODIE and SOPHIE archives we extracted available high-resolution spectra and RV measurements, along with RVs from the Lick planet search program. We combined our multi-epoch astrometry with these archival, partially unpublished RVs, and found that the comp

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9

Arenas, Villarroel Jose L. "Spectroscopy of the nova-like system UX UMa and three classical novae : V603 Aql, BT Mon and V1425 Aql." Thesis, Keele University, 2000. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.341306.

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10

Kellogg, Kendra, L. Prato, Guillermo Torres, et al. "The TWA 3 Young Triple System: Orbits, Disks, Evolution." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625499.

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We have characterized the spectroscopic orbit of the TWA 3A binary and provide preliminary families of probable solutions for the TWA 3A visual orbit, as well as for the wide TWA 3A-B orbit. TWA 3 is a hierarchical triple located at 34 pc in the similar to 10 Myr old TW Hya association. The wide component separation is 1."55; the close pair was first identified as a possible binary almost 20 years ago. We initially identified the 35-day period orbital solution using high-resolution infrared spectroscopy that angularly resolved the A and B components. We then refined the preliminary orbit by co

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11

Martinez, Arturo O., Ian J. M. Crossfield, Joshua E. Schlieder, et al. "Stellar and Planetary Parameters for K2's Late-type Dwarf Systems from C1 to C5." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623204.

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The NASA K2 mission uses photometry to find planets transiting stars of various types. M dwarfs are of high interest since they host more short-period planets than any other type of main-sequence star and transiting planets around M dwarfs have deeper transits compared to other main-sequence stars. In this paper, we present stellar parameters from K and M dwarfs hosting transiting planet candidates discovered by our team. Using the SOFI spectrograph on the European Southern Observatory's New Technology Telescope, we obtained R approximate to 1000 J-, H-, and K-band (0.95-2.52 mu m) spectra of

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12

Garcia, E. Victor, Thayne Currie, Olivier Guyon, et al. "SCExAO AND GPI Y JH BAND PHOTOMETRY AND INTEGRAL FIELD SPECTROSCOPY OF THE YOUNG BROWN DWARF COMPANION TO HD 1160." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623097.

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We present high signal-to-noise ratio, precise Y JH photometry and Y band (0.957-1.120 mu m) spectroscopy of HD 1160 B, a young substellar companion discovered from the Gemini NICI Planet Finding Campaign using the Subaru Coronagraphic Extreme Adaptive Optics instrument and the Gemini Planet Imager. HD 1160 B has typical mid-M dwarf-like infrared colors and a spectral type of M5.5(-0.5)(+1.0), where the blue edge of our Y band spectrum rules out earlier spectral types. Atmospheric modeling suggests HD 1160 B has an effective temperature of 3000-3100 K, a surface gravity of log g - 4-4.5, a rad

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13

Christiansen, Jessie L., Andrew Vanderburg, Jennifer Burt, et al. "Three’s Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/625817.

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HD 3167 is a bright (V = 8.9), nearby KO star observed by the NASA K2 mission (EPIC 220383386), hosting two small, short-period transiting planets. Here we present the results of a multi-site, multi-instrument radial-velocity campaign to characterize the HD 3167 system. The masses of the transiting planets are 5.02 +/- 0.38 M-circle plus for HD 3167 b, a hot super-Earth with a likely rocky composition (rho(b) = 5.6(-1.43)(+2.15) g cm(-3)), and 9.80(-1.24)(+1.30) M-circle plus for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement (rho(c) = 1.97(-0.59)(+0.94) g cm(-3)).

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14

De, Rosa Robert J., Julien Rameau, Jenny Patience, et al. "SPECTROSCOPIC CHARACTERIZATION OF HD 95086 b WITH THE GEMINI PLANET IMAGER." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621382.

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We present new H (1.51.8 mu m) photometric and K-1 (1.92.2 mu m) spectroscopic observations of the young exoplanet HD 95086 b obtained with the Gemini Planet Imager. The Hband magnitude has been significantly improved relative to previous measurements, whereas the lowresolution K-1 (lambda/delta lambda approximate to 66) spectrum is featureless within the measurement uncertainties and presents a monotonically increasing pseudocontinuum consistent with a cloudy atmosphere. By combining these new measurements with literature L' photometry, we compare the spectral energy distribution (SED) of the

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15

Sinukoff, Evan, Andrew W. Howard, Erik A. Petigura, et al. "ELEVEN MULTIPLANET SYSTEMS FROM K2 CAMPAIGNS 1 AND 2 AND THE MASSES OF TWO HOT SUPER-EARTHS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621388.

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We present a catalog of 11 multiplanet systems from Campaigns 1 and 2 of the K2 mission. We report the sizes and orbits of 26 planets split between seven two-planet systems and four three-planet systems. These planets stem from a systematic search of the K2 photometry for all dwarf stars observed by K2 in these fields. We precisely characterized the host stars with adaptive optics imaging and analysis of high-resolution optical spectra from Keck/HIRES and medium-resolution spectra from IRTF/SpeX. We confirm two planet candidates by mass detection and validate the remaining 24 candidates to >99

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16

Ramm, David John. "A spectroscopic study of detached binary systems using precise radial velocities." Thesis, University of Canterbury. Physics and Astronomy, 2004. http://hdl.handle.net/10092/1525.

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Spectroscopic orbital elements and/or related parameters have been determined for eight binary systems, using radial-velocity measurements that have a typical precision of about 15 ms⁻¹. The orbital periods of these systems range from about 10 days to 26 years, with a median of about 6 years. Orbital solutions were determined for the seven systems with shorter periods. The measurement of the mass ratio of the longest-period system, HD217166, demonstrates that this important astrophysical quantity can be estimated in a model-free manner with less than 10% of the orbital cycle observed spectrosc

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17

Neves, Vasco de Matos Ferreira Mendes. "Abundances of elements in exoplanet host stars." Master's thesis, Universidade de Aveiro, 2008. http://hdl.handle.net/10773/15237.

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Mestrado em Física<br>In this work we present an uniform study of the chemical abundances of 12 elements (Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Na, Mg and Al) derived from the spectra of 451 stars of one of the HARPS GTO planet search programs, which has 66 planet bearing stars. The main goal of this study is the investigation of the possible differences between the abundances of the stars with and without planets. We have confirmed that there is an overabundance of metallicity in planet host stars, common to all species, as expected. We have also found that there is no difference in the g

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18

Fischer, Patrick D., Heather A. Knutson, David K. Sing, et al. "HST HOT-JUPITER TRANSMISSION SPECTRAL SURVEY: CLEAR SKIES FOR COOL SATURN WASP-39b." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621278.

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We present the. Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) optical transmission spectroscopy of the cool Saturn-mass exoplanet WASP-39b from 0.29-1.025 mu m, along with complementary transit observations from Spitzer IRAC at 3.6 and 4.5 mu m. The low density and large atmospheric pressure scale height of WASP-39b make it particularly amenable to atmospheric characterization using this technique. We detect a Rayleigh scattering slope as well as sodium and potassium absorption features; this is the first exoplanet in which both alkali features are clearly detected w

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19

Ozbey, Mehtap. "The Optical Spectroscopic And Photometric Observations Of The Optical Counterparts To The Be/x-ray Binary Systems: Gro J2058+42 And V0332+53." Master's thesis, METU, 2008. http://etd.lib.metu.edu.tr/upload/12609774/index.pdf.

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The spectroscopic and photometric observations of the optical counterparts to the Be/X-ray binary systems GRO J2058+42 and V0332+53 (BQ Cam), taken with RTT150 (Russian-Turkish 1.5 meter Telescope), are presented in this study. The distance, color and the reddening estimates for both sources, obtained via photometric observations, are consistent with the previous results. The results of our spectroscopic observations performed between May 2006 and June 2008 for optical counterpart to GRO J2058+42 indicate that the double-peaked emission line profile turns into a single-peaked emission after th

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20

Dallow, Andrew Thomas. "Investigating the Enigmatic Orbit of the Suspected 2.5 MJ Planet in the Nu Octantis Binary System." Thesis, University of Canterbury. Physics and Astronomy, 2012. http://hdl.handle.net/10092/10364.

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ν Octantis is a spectroscopic binary with a semi-major axis and period of 2.55 AU and 2.9 years, respectively. Ramm et al. (2009) discovered a 52 ms^(-1) radial-velocity (RV) perturbation with a period of 417 days in this system. All evidence, both photometric and spectroscopic, suggests the perturbation is the result of a 2.5 MJ planet orbiting the primary star. However, when assuming a “normal” prograde coplanar orbit, celestial mechanics predicts this orbit is unstable, contradicting the observed stability. Simulations by Eberle and Cuntz (2010) showed a retrograde orbit for the planet to

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21

Lothringer, Joshua D., Björn Benneke, Ian J. M. Crossfield, et al. "An HST/STIS Optical Transmission Spectrum of Warm Neptune GJ 436b." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/626526.

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GJ 436b is a prime target for understanding warm Neptune exoplanet atmospheres and a target for multiple James Webb Space Telescope (JWST) Guaranteed Time Observation programs. Here, we report the first space-based optical transmission spectrum of the planet using two Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) transit observations from 0.53 to 1.03 mu m. We find no evidence for alkali absorption features, nor evidence of a scattering slope longward of 0.53 mu m. The spectrum is indicative of moderate to high metallicity (similar to 100-1000x solar), while moderate

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22

Gullikson, Kevin Carl. "Towards spectroscopic detection of low mass ratio stellar binary systems." Thesis, 2012. http://hdl.handle.net/2152/ETD-UT-2012-08-6275.

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Detection of the emission from the secondary component in a binary system can be extremely challenging, but equally rewarding. In the case of intermediate to high-mass binaries, detection of close companions can inform formation theories. In the extreme low mass-ratio case, where the secondary component is in fact a planet, detection of the emission in high resolution spectroscopy can be used to determine the true planet mass. In this thesis, we describe a technique to detect the thermal emission from the secondary component of a low mass-ratio binary system. We apply this technique to archive

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23

Veicht, Aaron Michael. "Through the Forest of Speckles: Robust Spectroscopy of Extremely Faint Companions of Nearby Stars." Thesis, 2016. https://doi.org/10.7916/D8TT4QWM.

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The discovery and characterization of exoplanetary systems is a new exciting field. At just over two decades old, it has already fundamentally reshaped our knowledge of planet and solar system formation. We now know that there is a vast diversity of planetary systems, in highly varied, even bizarre, configurations. Known planetary bodies span all masses from objects less massive and smaller than Earth to objects as large as the smallest stars or brown dwarfs. They exhibit periods of but a few hours to periods spanning millennia, from nearly perfectly circular orbits to highly elliptical, from

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24

Themeẞl, Nathalie. "Asteroseismic inferences from red-giant stars." Doctoral thesis, 2018. http://hdl.handle.net/11858/00-1735-0000-002E-E5F1-E.

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25

Jofré, Jorge Emiliano. "Estrellas evolucionadas con planetas : abundancias químicas y propiedades planetarias." Doctoral thesis, 2015. http://hdl.handle.net/11086/2865.

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Tesis (Doctor en Astronomía)--Universidad Nacional de Córdoba, Facultad de Matemática, Astronomía y Física, 2015.<br>Actualmente es un hecho aceptado que las estrellas de secuencia principal que albergan planetas gigantes son, en promedio, más ricas en metales que aquéllas sin planetas detectados. Sin embargo, en el caso de las estrellas evolucionadas, especialmente las gigantes, los resultados han sido más dispares o controversiales por lo que el tema permanece abierto. Por otro lado, aún se debate fuertemente si las estrellas de secuencia principal con planetas gigantes poseen menor abundanc

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26

Lovos, Flavia Virginia. "Estudio de variabilidad fotométrica en estrellas de tipo T Tauri." Doctoral thesis, 2019. http://hdl.handle.net/11086/14315.

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Tesis (Doctor en Astronomía)--Universidad Nacional de Córdoba, Facultad de Matemática, Astronomía, Física y Computación, 2019.<br>Las estrellas jóvenes de tipo T Tauri tienen la edad adecuada para el inicio del proceso de formación planetaria de acuerdo a los modelos más aceptados en la actualidad. Sin embargo éstas presentan algunos desafíos para la técnica clásica de detección de planetas extrasolares mediante tránsitos planetarios. Principalmente las T Tauri manifiestan diversas formas de variabilidad que, mayormente, se evidencian en sus curvas de luz. En este trabajo se presenta un anális

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27

Petrucci, Romina Paola. "Estudio de variaciones en los tiempos de mínimo en estrellas con planetas transitantes del Hemisferio Sur." Doctoral thesis, 2015. http://hdl.handle.net/11086/2868.

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Tesis (Doctor en Astronomía)--Universidad Nacional de Córdoba, Facultad de Matemática, Astronomía y Física, 2015.<br>En este trabajo presentamos los resultados del monitoreo y análisis homogéneo de tránsitos de planetas que orbitan alrededor de estrellas del Hemisferio Sur. El propósito principal de este seguimiento fotométrico es el de buscar variaciones en los tiempos de mínimo (TTVs) que pudieran atribuirse a la presencia de otros cuerpos de masa planetaria no detectados, ligados gravitacionalmente al sistema. Para ello realizamos observaciones con los telescopios argentinos Horacio Ghielm

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