Relevant bibliographies by topics / Star system spectroscopy

Contents

  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers

Academic literature on the topic 'Star system spectroscopy'

Author: Grafiati
Published: 4 June 2021
Last updated: 1 February 2022

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Journal articles on the topic "Star system spectroscopy"

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Hinkle, Kenneth H., Stephen T. Ridgway, and Francis C. Fekel. "Infrared Spectroscopy of Multiple Star Systems." International Astronomical Union Colloquium 135 (1992): 149–51. http://dx.doi.org/10.1017/s0252921100006266.

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AbstractUp to this time infrared spectroscopy has been only occasionally used in binary star research due to both the insensitivity of infrared spectrographs and the difficulty of getting observing time on a limited number of spectrographs. However, infrared spectroscopy has a number of interesting applications in binary star research. We present an example of an application to the long-period symbiotic system CH Cyg. Due to the recent development of infrared arrays, infrared spectroscopy (1) is becoming available at a much larger number of telescopes and (2) in the 1.0-2.5 μm region is capable of going to limiting magnitudes nearly as faint as those reached by CCD’s.
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Maíz Apellániz, J., R. H. Barbá, S. Simón-Díaz, A. Sota, E. Trigueros Páez, J. A. Caballero, and E. J. Alfaro. "Lucky Spectroscopy, an equivalent technique to Lucky Imaging." Astronomy & Astrophysics 615 (July 2018): A161. http://dx.doi.org/10.1051/0004-6361/201832885.

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Context. Many massive stars have nearby companions whose presence hamper their characterization through spectroscopy. Aims. We want to obtain spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. Methods. We obtained a large number of short long-slit spectroscopic exposures of five close binaries under good seeing conditions. We selected those with the best characteristics, extracted the spectra using multiple-profile fitting, and combined the results to derive spatially separated spectra. Results. We demonstrate the usefulness of Lucky Spectroscopy by presenting the spatially resolved spectra of the components of each system, in two cases with separations of only ~0.′′3. Those are δ Ori Aa+Ab (resolved in the optical for the first time) and σ Ori AaAb+B (first time ever resolved). We also spatially resolve 15 Mon AaAb+B, ζ Ori AaAb+B (both previously resolved with GOSSS, the Galactic O-Star Spectroscopic Survey), and η Ori AaAb+B, a system with two spectroscopic B+B binaries and a fifth visual component. The systems have in common that they are composed of an inner pair of slow rotators orbited by one or more fast rotators, a characteristic that could have consequences for the theories of massive star formation.
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Charles, P. A. "Black-Hole Systems: Optical Spectroscopy and IR Photometry." Symposium - International Astronomical Union 165 (1996): 341–50. http://dx.doi.org/10.1017/s0074180900055807.

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The X-ray transient systems have provided the first opportunities for detailed studies of the mass losing star in low-mass X-ray binaries. During X-ray quiescence the cool star is the dominant light source in the red and near-IR. Optical spectroscopy yields the mass function (itself a lower limit to the compact-object mass), the rotational broadening leads to the mass ratio, q (assuming only that the star fills its Roche lobe), and the IR ellipsoidal light curve gives the system inclination (for high q). In such cases, a complete solution to the system parameters is possible, and this has been performed for A 0620-00 (V616 Mon) and GS 2023+338 (V404 Cyg), leading to the first accurate black-hole masses (which are in the range 10–12 M⊙).
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Moffat, Anthony F. J. "Time-resolved optical-UV spectroscopy of colliding wind effects." Symposium - International Astronomical Union 193 (1999): 278–88. http://dx.doi.org/10.1017/s0074180900205548.

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It is in the ultraviolet-optical domain where the strongest known emission lines arise in hot star winds. In the case of hot-star binaries, culminating in the relatively common, strong-wind WR+O systems, similar line-emission is seen in the cooling flows downstream from the highly compressed, X-ray emitting heads of the bow shock regions produced when the two winds collide. Time-resolved UV-optical spectroscopy of these flows around a complete orbit can provide important constraints not only on the colliding wind process itself, but also on the winds and the orbit. Spectroscopic wind-wind collision effects have now been seen in every relatively close WR+O system (P ≲ 100 d) that has been adequately observed so far.
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Hajduk, Marcin, Peter A. M. van Hoof, and Albert A. Zijlstra. "GLMP 160 – the first [WR] star in a binary." Proceedings of the International Astronomical Union 7, S283 (July 2011): 382–83. http://dx.doi.org/10.1017/s1743921312011532.

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AbstractWe discuss the results of the search for [WR] central stars in binary systems. GLMP 160 is the first [WR] central star in a binary system known. We analyze photometry, spectroscopy and imaging of this system.
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Walton, N. A., J. R. Walsh, and S. R. Pottasch. "Imaging and Spectroscopy of Abell 63 (UU SGE)." Symposium - International Astronomical Union 155 (1993): 394. http://dx.doi.org/10.1017/s0074180900171839.

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UU Sge, the eclipsing binary central star (Bond et al, 1978) of the low-surface-brightness planetary nebula (PN) Abell 63, has been observed spectroscopically in the visible throughout its 11.2 hour period and especially during the minimum. A spectral determination of the binary system has been made. The primary hot central star is an ‘O’ type PN nucleus of temperature ≈40,000 K, consistent with the low excitation of the nebular spectrum (e.g. no He ii 4686Å nebular emission detected). From the spectrum at minimum light, the secondary star appears to be a cool dwarf star around G7. Measurement of the magnitude of the secondary during the eclipse of the primary enabled the distance to the PN to be directly determined as 3.6 kpc. For this distance the luminosity of the hot star is approximately 4 320 L⊙, in good agreement with evolutionary tracks for (single) PN nuclei. Deep CCD images of Abell 63 show it has a ‘butterfly’ morphology implying that the close binary central system may have had a strong effect on the nebula shaping. The paper describing this work has been submitted (Walton et al, 1992).
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Skopal, A., D. Chochol, A. Vittone, and A. Mammano. "Photometric and Spectroscopic Variations of the Symbiotic Star EG Andromedae." International Astronomical Union Colloquium 103 (1988): 289–90. http://dx.doi.org/10.1017/s0252921100103665.

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EG And is a symbiotic binary system. The cool component is an M3 III star, the hot one is a subdwarf with temperature 60 250 K and luminosity 1.45 L⊙ (Boyarchuk, 1985). The eclipsing nature of the system suggested from UV spectroscopy by Oliversen et al. (1985) was confirmed photometrically by Chochol et al. (1987). The circular spectroscopic orbit of cool component determined by Oliversen et al. (1985) supposing the orbital period 470 days leads to f(m) = 3.2×10−2 M⊙ and detached configuration.
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Hummel, Christian A. "Imaging and Modeling of Double Stars with the Navy Prototype Optical Interferometer: a Continuation of the Mark III Double Star Program." International Astronomical Union Colloquium 170 (1999): 416–21. http://dx.doi.org/10.1017/s0252921100048855.

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AbstractWe present results from the new Navy Prototype Optical Interferometer (NPOI) – the orbit of the double star Mizar A and measurements of Matar – which are compared to an orbit determined with the predecessor of NPOI, the Mark III Interferometer. Uncertainties of the orbital inclination are between 0.1 and 0.3 degrees; those of the semi-major axis are less than 0.5 percent. We determine the component masses and other parameters of the double star system, including relative photometry, directly through a fit to a combination of interferometric and spectroscopic data. Algorithms were developed to handle any hierarchical stellar system.We describe plans for the study of spectroscopic double stars with NPOI, which draw from our experience with the Mark III binary program. This program yielded orbits of 26 stars, of which 17 were published with mass determinations of 24 components using spectroscopy. The accuracy of the physical parameters were often limited by the spectroscopy. We show that in order to benefit from the high precision of the interferometric observations, new high-precision spectroscopic observations, combined with improved algorithms for the detection of the secondaries, are required.
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Hinkle, Kenneth H., Francis C. Fekel, Richard R. Joyce, Joanna Mikołajewska, Cezary Gałan, and Thomas Lebzelter. "Infrared Spectroscopy of Symbiotic Stars. XII. The Neutron Star SyXB System 4U 1700+24 = V934 Herculis." Astrophysical Journal 872, no. 1 (February 8, 2019): 43. http://dx.doi.org/10.3847/1538-4357/aafba5.

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Davis, John. "Overview of Multiple–Aperture Interferometry Binary Star Results from the Southern Hemisphere." Proceedings of the International Astronomical Union 2, S240 (August 2006): 45–53. http://dx.doi.org/10.1017/s174392130700378x.

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AbstractThe first multiple-aperture interferometric study of a binary system, in which the power of combining interferometric and spectroscopic data was demonstrated, was made from the Southern Hemisphere. The observations of α Vir with the Narrabri Stellar Intensity Interferometer (NSII) were combined with spectroscopic and photometric data to yield the mass, radius and luminosity of the primary as well as an accurate distance to the system. The NSII also revealed a number of stars, previously thought to be single, to be binary systems. Several of these systems have subsequently been shown to be spectroscopic binaries.The Sydney University Stellar Interferometer (SUSI) and the European Southern Observatory's Very Large Telescope Interferometer (VLTI) are the two current Southern Hemisphere multiple aperture interferometers. SUSI is being used to determine interferometric orbits for some of the binary systems discovered with the NSII including β Cen and λ Sco and, in combination with spectroscopy, to determine accurate masses for early-type stars and accurate dynamical parallaxes for the systems.The VLTI has operated with three beam-combining instruments, namely VINCI, MIDI and AMBER. The few observations of binary systems that have been made so far are summarised and, while in general they are of a preliminary nature, they demonstrate the potential of the VLTI for binary star studies.One double-lined spectroscopic binary that has been observed with all three Southern Hemisphere instruments is γ2 Vel, which has the brightest Wolf-Rayet star in the sky as its secondary. The observations and preliminary results for the masses of the O-type primary and WC8 secondary and for the distance to the system are summarised.
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Dissertations / Theses on the topic "Star system spectroscopy"

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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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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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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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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 lines. Cataclysmic variable stars in which the magnetic field is strong enough to prevent the formation of the accretion disk are called AM Herculis-type systems, after their prototype. In this study, the time-resolved spectroscopy of two AM Herculis-type binary systems, QQ Vul and EF Eri, are analyzed. In addition, Doppler Tomography, an analysis technique previously applied primarily to cataclysmic variable stars with accretion disks, is applied to these systems.
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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/B). J’ai déterminé l’intervalle de S/B dans lequel un spectre stellaire est fiable pour la mesure des paramètres stellaires.Dans le cadre du consortium SOPHIE, j’ai suivi l’analyse complète du système Kepler-117. Ce système multi-planétaire montre variations des périodes orbitaux dues aux échanges dynamiques entre les planètes (TTV). Pour déterminer les paramètres du système, un approche spécifique a été développé pour l’ajustement simultané de transits, VR et TTV (Bruno et al. 2015).Finalement, je me suis intéressé à l’activité stellaire dans la photométrie de transit. J’ai impl ́ementé deux logiciels de modélisation de tâches stellaires dans un code MCMC, en ajoutant l’évolution des tâches dans l’un d’eux. J’ai appliqué les logiciels au Soleil, à CoRoT-7 et à CoRoT-2. J’ai amené un étude détaillé de la courbe de lumière de CoRoT-2, et exploré les effets des tâches dans les paramètres du transit (Bruno et al., en prep.). Avec la méthode FF’ (Aigrain et al. 2012), j’ai contribué à l’exploration du lien entre la signature des tâches de CoRoT-7 et dans la photométrie et dans les VR
During my PhD, I analyzed the spectra of nine Kepler stars obtained by radial velocity (RV) observations. This allowed the characterization of their planetary companions. I analyzed the spectra of twenty-one other CoRoT and Kepler stars, likely orbited by low-mass M dwarfs. This helped widening the sample of low-mass stars with measured mass and radius. I calculated the chromospheric activity indfex of thirty-one stars observed with SOPHIE/OHP, helping the study of star-planet interactions. I studied the behavior of SOPHIE in low signal-to-noise ratio (SNR) regime. I determinhed the SNR range in which a stellar spectrum is reliable for the measure of the stellar parameters.Within the SOPHIE consortium, I followed the complete analysis of the Kepler-117 system. This multi-planetary system presents variations in the planetary orbital periods due to their mutual dynamical interacion (TTVs). To fit the system parameters, a specific fitting approach including TTV modeling was developed. We derived the system parameters by the simultaneous fit of transits, RVs, and TTVs (Bruno et al. 2015).Finally, I addressed the problem of stellar activity in transit photometry. I implemented two starspot modeling codes into an MCMC algorithm, adding spot evolution to oneof them. I applied the codes to the Sun, CoRoT-7, and CoRoT-2. I carried an extensive study on the light curve of CoRoT-2, and explored the effects of the spots on the transit parameters (Bruno et al., in prep.). With the FF’ method (Aigrain et al. 2012), I contributed to explore the connection between the photometric and RV signature of starspots in CoRoT-7
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Johnson-Groh, Mara, Christian Marois, Rosa Robert J. De, Eric L. Nielsen, Julien Rameau, Sarah Blunt, Jeffrey Vargas, 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 address the considerable spectral covariance in both spectra, we present a method of splitting the spectra into low and high frequencies to analyze the spectral structure at different spatial frequencies with the proper spectral noise correlation. Using the split spectra, we compare them to known spectral types using field brown dwarf and low-mass star spectra and find a best-fit match of a field gravity M6.5 +/- 1.5 spectral type with a corresponding temperature of 2730(-180)(+120)K. Photometry of the companion yields a luminosity of log(L-bol/L-circle dot) = -2.88 +/- 0.07 dex with DUSTY models. Mass estimates, again from DUSTY models, find an age-dependent mass of 34 +/- 1 to 95 +/- 4 M-Jup. These results are consistent with previous measurements of the object.
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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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Hełminiak, K. G., M. Kuzuhara, K. Mede, T. D. Brandt, R. Kandori, T. Suenaga, N. Kusakabe, 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 companion is a low-mass star, not a brown dwarf, as previously suggested. We found the best-fitting dynamical masses to be m(1) = 1.141(-0.091)(+0.037)and m(2) = 0.279(-0.020)(+0.023) M-circle dot. We also performed spectral analysis of the SOPHIE spectra with the iSpec code. Hipparcos time-series photometry shows a periodicity of P = 5.743 day, which is also seen in the SOPHIE spectra as an RV modulation of the star A. We interpret it as being caused by spots on the stellar surface, and the star to be rotating with the given period. From the rotation and level of activity, we found that the system is 380(-100)(+220) Myr old, consistent with an isochrone analysis (220(-90)(+2120) Myr). This work may serve as a test case for future studies of low-mass stars, brown dwarfs, and exoplanets by combination of RV and direct imaging data.
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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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Kellogg, Kendra, L. Prato, Guillermo Torres, G. H. Schaefer, I. Avilez, D. Ruíz-Rodríguez, L. H. Wasserman, 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 combining the infrared data with a reanalysis of our high-resolution optical spectroscopy. The orbital period from the combined spectroscopic solution is similar to 35 days, the eccentricity is similar to 0.63, and the mass ratio is similar to 0.84; although this high mass ratio would suggest that optical spectroscopy alone should be sufficient to identify the orbital solution, the presence of the tertiary B component likely introduced confusion in the blended optical spectra. Using millimeter imaging from the literature, we also estimate the inclinations of the stellar orbital planes with respect to the TWA 3A circumbinary disk inclination and find that all three planes are likely misaligned by at least similar to 30 degrees. The TWA 3A spectroscopic binary components have spectral types of M4.0 and M4.5; TWA 3B is an M3. We speculate that the system formed as a triple, is bound, and that its properties were shaped by dynamical interactions between the inclined orbits and disk.
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Books on the topic "Star system spectroscopy"

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Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (13th 2004 Hamburg, Germany). Proceedings of the 13th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun: 5-9 July 2004, Hamburg, Germany. Noordwijk, The Netherlands: ESA Publication Division, 2005.

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Stern, Robert A. [Theta]¹ and [gamma] Tauri, understanding the coronal structure of Hyades giants: EUV spectroscopy of BY Dra systems : combined final report. [Washington, D.C: National Aeronautics and Space Administration, 1995.

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Black, David C. Completing the copernican revolution: The search for other planetary systems. [Washington, DC: National Aeronautics and Space Administration, 1995.

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Nanda, Rea, and SpringerLink (Online service), eds. High-Energy Emission from Pulsars and their Systems: Proceedings of the First Session of the Sant Cugat Forum on Astrophysics. Berlin, Heidelberg: Springer-Verlag Berlin Heidelberg, 2011.

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Polarimetry of Stars and Planetary Systems. Cambridge University Press, 2015.

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United States. National Aeronautics and Space Administration., ed. Completing the copernican revolution: The search for other planetary systems. [Washington, DC: National Aeronautics and Space Administration, 1995.

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Torres, Diego F., and Nanda Rea. High-Energy Emission from Pulsars and their Systems: Proceedings of the First Session of the Sant Cugat Forum on Astrophysics. Springer, 2013.

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Book chapters on the topic "Star system spectroscopy"

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Massey, Philip, and Margaret M. Hanson. "Astronomical Spectroscopy." In Planets, Stars and Stellar Systems, 35–98. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5618-2_2.

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Elnaggar, Hebatalla, Pieter Glatzel, Marius Retegan, Christian Brouder, and Amélie Juhin. "X-ray Dichroisms in Spherical Tensor and Green’s Function Formalism." In Springer Proceedings in Physics, 83–130. Cham: Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-64623-3_4.

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AbstractIn this book chapter, our goal is to provide experimentalists and theoreticians with an accessible approach to the measurement or calculation of X-ray dichroisms in X-ray absorption spectroscopy (XAS). We start by presenting the key ideas of different calculation methods such as density functional theory (DFT) and ligand-field multiplet (LFM) theory and discuss the pros and cons for each approach. The second part of the chapter is dedicated to the expansion of the XAS cross section using spherical tensors for electric dipole and quadrupole transitions. This expansion enables to identify a set of linearly independent spectra that represent the smallest number of measurements (or calculations) to be performed on a sample, in order to extract all spectroscopic information. Examples of the different dichroic effects which can be expected depending on the type of transitions and on the symmetry of the system are then given.
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Charles, P. A. "Black-Hole Systems: Optical Spectroscopy and IR Photometry." In Compact Stars in Binaries, 341–50. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0167-4_30.

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Vilhu, O., B. Gustafsson, and B. Edvardsson. "Spectroscopy of the rapidly rotating K-star HD 36705." In Cool Stars, Stellar Systems, and the Sun, 268–70. Berlin, Heidelberg: Springer Berlin Heidelberg, 1986. http://dx.doi.org/10.1007/3-540-16763-3_193.

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Eggenberger, Anne, and Stéphane Udry. "Probing the Impact of Stellar Duplicity on Planet Occurrence with Spectroscopic and Imaging Observations." In Planets in Binary Star Systems, 19–49. Dordrecht: Springer Netherlands, 2010. http://dx.doi.org/10.1007/978-90-481-8687-7_2.

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Hinkle, Kenneth H., and Werner W. G. Scharlach. "Time series infrared spectroscopy of long period variables." In Cool Stars, Stellar Systems, and the Sun, 387–89. Berlin, Heidelberg: Springer Berlin Heidelberg, 1987. http://dx.doi.org/10.1007/3-540-18653-0_162.

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Sylvester, R. J., M. J. Barlow, and C. J. Skinner. "Millimetre Photometry and Infrared Spectroscopy of Vega-Excess Stars." In Planetary Systems: Formation, Evolution, and Detection, 261–70. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1154-6_28.

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Dupree, A. K., S. L. Baliunas, E. F. Guinan, L. Hartmann, and G. S. Sonneborn. "Recent spectroscopic observations of Alpha Orionis." In Cool Stars, Stellar Systems, and the Sun, 411–13. Berlin, Heidelberg: Springer Berlin Heidelberg, 1986. http://dx.doi.org/10.1007/3-540-16763-3_223.

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Foing, B., J. Beckman, L. Crivellari, G. Vladilo, and S. Char. "Spectroscopic variability associated with chromospheric activity: The α CEN system." In Cool Stars, Stellar Systems, and the Sun, 488–91. Berlin, Heidelberg: Springer Berlin Heidelberg, 1986. http://dx.doi.org/10.1007/3-540-16763-3_244.

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Herczeg, T. J. "A Survey of Third Components in Spectroscopic and Eclipsing Systems." In Wide Components in Double and Multiple Stars, 89–95. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2987-6_15.

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Conference papers on the topic "Star system spectroscopy"

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Goto, Tomotsugu, M. Yagi, C. Yamauchi, Victor P. Debattista, and C. C. Popescu. "Cosmic Star Formation History Revealed by the Akari & Spatially-Resolved Spectroscopy of an E+A (Post-Starburst) System." In HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. AIP, 2010. http://dx.doi.org/10.1063/1.3458562.

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2

Jeong, Do-Young, K. S. Lee, A. S. Choe, Jongmin Lee, and Bum Ku Rhee. "Dynamic Stark shift in a 3-level atomic system." In Resonance ionization spectroscopy 1996: Eighth international symposium. AIP, 1997. http://dx.doi.org/10.1063/1.52154.

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3

Smirnova, O., L. Začs, O. Alksnis, F. Musaev, and Eric Stempels. "The Spectroscopy of the Pulsating Carbon Stars." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099258.

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4

Ak, N. Filiz, Z. Eker, H. Ak, I. Küçük, and Eric Stempels. "High Resolution Coude Echelle Spectroscopy of IX Per." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099193.

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5

Krötz, Peter, Guido Sonnabend, Manuela Sornig, Dušan Stupar, Rudolf Schieder, and Eric Stempels. "Probing Stellar Atmospheres with Ultra-High Resolution Infrared Heterodyne Spectroscopy." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099282.

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6

Barnes, J. R., Travis S. Barman, H. R. A. Jones, C. J. Leigh, A. Collier Cameron, Lisa Prato, R. Barber, and Eric Stempels. "Spectroscopic Characterisation of Close Orbiting Extrasolar Giant Planets." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099136.

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7

Neuhäuser, Ralph, Tobias O. B. Schmidt, Andreas Seifahrt, Ana Bedalov, Christiane Helling, Sören Witte, Peter Hauschildt, and Eric Stempels. "Medium-resolution infrared integral field spectroscopy of the brown dwarf TWA 5 B." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099248.

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8

Maldonado, J., R. M. Martínez-Arnáiz, C. Eiroa, D. Montes, and Eric Stempels. "Spectroscopic Studies of Nearby Cool Stars: The DUNES Sample." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099135.

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9

Albert, Loïc, Étienne Artigau, Philippe Delorme, Xavier Delfosse, Thierry Forveille, Céline Reylé, Chris Willott, and Eric Stempels. "Spectroscopic Follow-up of the CFBDS T Dwarf Candidates." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099154.

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10

Fekel, Francis C., B. Zuckerman, Michael H. Williamson, Gregory W. Henry, M. P. Muno, and Eric Stempels. "The Dusty, Solar Type Spectroscopic Binary BD +20 307." In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099246.

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