Relevant bibliographies by topics / Stars with planets

Academic literature on the topic 'Stars with planets'

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Published: 4 June 2021
Last updated: 5 February 2022

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Journal articles on the topic "Stars with planets"

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MacCAIG, Norman. "Stars and planets." Medicine, Conflict and Survival 14, no. 3 (July 1998): 272. http://dx.doi.org/10.1080/13623699808409404.

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Hirano, Teruyuki, Bun'ei Sato, Kento Masuda, Othman Michel Benomar, Yoichi Takeda, Masashi Omiya, and Hiroki Harakawa. "Search for Close-in Planets around Evolved Stars with Phase-curve variations and Radial Velocity Measurements." Proceedings of the International Astronomical Union 11, A29A (August 2015): 63–64. http://dx.doi.org/10.1017/s1743921316002404.

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AbstractTidal interactions are a key process to understand the evolution history of close-in exoplanets. But tidals still have a large uncertainty in their prediction for the damping timescales of stellar obliquity and semi-major axis. We have worked on a search for transiting giant planets around evolved stars, for which few close-in planets were discovered. It has been reported that evolved stars lack close-in planets, which is often attributed to the tidal evolution and/or engulfment of close-in planets by the hosts. Meanwhile, Kepler has detected a certain fraction of transiting planet candidates around evolved stars. Confirming the planetary nature for these candidates is especially important since the comparison between the occurrence rates of close-in planets around main sequence stars and evolved stars provides a unique opportunity to discuss the final stage of close-in planets. With the aim of confirming KOI planet candidates around evolved stars, we measured precision radial velocities (RVs) for evolved stars with transiting planet candidates using Subaru/HDS. We also developed a new code which simultaneously models and fits the observed RVs and phase-curve variations in the Kepler data (e.g., transits, stellar ellipsoidal variations, and planet emission/reflected light). As a result of applying the global fit to KOI giants/subgiants, we confirmed two giant planets around evolved stars (Kepler-91 and KOI-1894), as well as revealed that KOI-977 is more likely a false positive.
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Carlberg, Joleen K., Steven R. Majewski, Verne V. Smith, Katia Cunha, Richard J. Patterson, Dmitry Bizyaev, Phil Arras, and Robert T. Rood. "A New Spin on Red Giant Rapid Rotators: Evidence for Chemical Exchange Between Planets and Evolved Stars." Proceedings of the International Astronomical Union 5, S265 (August 2009): 408–11. http://dx.doi.org/10.1017/s1743921310001092.

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AbstractRapid rotation in red giant stars may be one signature of the past engulfment of a planetary companion. Models of the future tidal interaction of known exoplanet host stars with their planets show that many of these stars will accrete one or more of their planets, and the orbital angular momentum of these accreted planets is sometimes sufficient to spin up the host stars to a level commonly accepted as “rapid rotation” for giant stars. Planets accreted during the red giant phase should leave behind a chemical signature in the form of unusual abundance patterns in the host red giant's atmosphere. Proposed signatures of planet accretion include the enhancement of Li and 12C; both species are generally depleted in giant star atmospheres by convection but could be replenished by planet accretion. Moreover, accreted planets may preferentially enhance the stellar abundance of refractory elements assuming that the refractory nature of these elements leads to their relative enhancements in the planets themselves. Here we present preliminary results of a search for these predicted chemical signatures through high resolution spectroscopic abundance analysis of both rapidly rotating giant stars (i.e., stars with a higher probability of having experienced planet accretion) and normally rotating giant stars. We find that the rapid rotators are enhanced in Li relative to the slow rotators — a result consistent with Li replenishment through planet absorption.
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Dvorak, R., E. Pilat-Lohinger, E. Bois, B. Funk, F. Freistetter, and L. Kiseleva-Eggleton. "Planets in Double Stars: The ϒ Cephei System." International Astronomical Union Colloquium 191 (August 2004): 222–26. http://dx.doi.org/10.1017/s0252921100008800.

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AbstractUp to now we have evidence for some 15 planets moving in double stars. They are all of the so-called S-type, which means that they are orbiting one of the primaries. Only two of the binaries have separations in the order of the distances where the planets in our Solar system orbit the Sun, namely Gliese 86 and ϒ Cep. In this study we investigate the stability of the recently discovered planet in ϒ Cep with respect to the orbital parameters of the binary and of the planet. Additionally we check the region inside and outside the planet’s orbit (a = 2.1 AU). Even when the mass of an additional planet in 1 AU would be in the order of that of Jupiter, the discovered planet would be in a stable orbit.
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Marcy, G. W., R. Paul Butler, and D. A. Fischer. "Doppler Detection of Extrasolar Planets." International Astronomical Union Colloquium 170 (1999): 121–30. http://dx.doi.org/10.1017/s0252921100048466.

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AbstractWe have measured the radial velocities of 540 G and K main sequence stars with a precision of 3−10 ms−1 using the Lick and Keck échelle spectrometers. We had detected 6 companions that have m sin i < 7 MJup. We announce here the discovery of a new planet around Gliese 876, found in our Doppler measurements from both Lick and Keck. This is the first planet found around an M dwarf, which indicates that planets occur around low-mass stars, in addition to solar-type stars. We combine our entire stellar sample with that of Mayor et al. to derive general properties of giant planets within a few AU of these stars. Less than 1% of G and K main sequence stars harbor brown dwarf companions with masses between 5 and 70 MJup. Including Gliese 876b, 8 companions exhibit m sin i < 5 MJup which constitute the best planet candidates to date. Apparently, 4% of stars have planetary companions within the range m sin i = 0.5 to 5 MJup. Planets are distinguished from brown dwarfs by the discontinuous jump in the mass function at 5 MJup. About 2/3 of the planets orbit within just 0.3 AU due in part to their favorable detectability, but also possibly due to a real “pile up” of planets near the star. Inward orbital migration after formation may explain this, but the mechanism to stop the migration remains unclear. Five of eight planets have orbital eccentricities greater than that of our Jupiter, eJup = 0.048, and tidal circularization may explain most of the circular orbits. Thus, eccentric orbits are common and may arise from gravitational interactions with other planets, stars, or the protoplanetary disk. The planet-bearing stars are systematically metal-rich, as is the Sun, compared to the solar neighborhood.
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Underwood, D. R., B. W. Jones, and P. N. Sleep. "The evolution of habitable zones during stellar lifetimes and its implications on the search for extraterrestrial life." International Journal of Astrobiology 2, no. 4 (October 2003): 289–99. http://dx.doi.org/10.1017/s1473550404001715.

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A stellar evolution computer model has been used to determine changes in the luminosity L and effective temperature Te of single stars during their time on the main sequence. The range of stellar masses investigated was from 0.5 to 1.5 times that of the Sun, each with a mass fraction of metals (metallicity, Z) from 0.008 to 0.05. The extent of each star's habitable zone (HZ) has been determined from its values of L and Te. These stars form a reference framework for other main sequence stars. All of the 104 main sequence stars known to have one or more giant planets have been matched to their nearest stellar counterpart in the framework, in terms of mass and metallicity, hence closely approximating their HZ limits. The limits of HZ, for each of these stars, have been compared to their giant planet(s)'s range of strong gravitational influence. This allows a quick assessment as to whether Earth-mass planets could exist in stable orbits within the HZ of such systems, both presently and at any time during the star's main sequence lifetime. A determination can also be made as to the possible existence of life-bearing satellites of giant planets, which orbit within HZs. Results show that about half of the 104 known extrasolar planetary systems could possibly have been housing an Earth-mass planet in HZs during at least the past billion years, and about three-quarters of the 104 could do so for at least a billion years at some time during their main sequence lives. Whether such Earth-mass planets could have formed is an urgent question now being investigated by others, with encouraging results.
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Beichman, C. A., S. C. Unwin, M. Shao, A. M. Tanner, J. H. Catanzarite, and G. W. Marcy. "Astrometric planet searches with SIM PlanetQuest." Proceedings of the International Astronomical Union 3, S248 (October 2007): 238–43. http://dx.doi.org/10.1017/s1743921308019169.

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AbstractSIM will search for planets with masses as small as the Earth's orbiting in the ‘habitable zones’ around more than 100 of the nearest stars and could discover many dozen if Earth-like planets are common. With a planned “Deep Survey” of 100–450 stars (depending on desired mass sensitivity) SIM will search for terrestrial planets around all of the candidate target stars for future direct detection missions such as Terrestrial Planet Finder and Darwin. SIM's “Broad Survey” of 2100 stars will characterize single and multiple-planet systems around a wide variety of stellar types, including many now inaccessible with the radial velocity technique. In particular, SIM will search for planets around young stars providing insights into how planetary systems are born and evolve with time.
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Hidas, M. G., J. K. Webb, M. C. B. Ashley, C. H. Lineweaver, J. Anderson, and M. Irwin. "Searching for Extrasolar Planets Using Transits." Symposium - International Astronomical Union 213 (2004): 77–79. http://dx.doi.org/10.1017/s0074180900193015.

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The presence of an extrasolar planet can be revealed when it passes in front of its host star, reducing the star's apparent brightness by ∼ 1%. We are monitoring a large sample (of order 104) of stars using our own 0.5 m telescope at Siding Spring Observatory, Australia, in search of such transiting planets.
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Gazzano, Jean-Christophe, Magali Deleuil, Patrick De Laverny, Alejandra Recio Blanco, François Bouchy, Davide Gandolfi, and Benoît Loeillet. "From stars to planets." Proceedings of the International Astronomical Union 4, S253 (May 2008): 404–5. http://dx.doi.org/10.1017/s174392130802677x.

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AbstractA large program of multi-fibre (FLAMES) spectroscopic observations of the stellar population in two CoRoT/Exoplanet field with the GIRAFFE/VLT, took place in spring 2008. It aims at characterizing the brightest dwarf population and providing the ground for statistical analysis of the planetary population found by CoRoT.To perform such an ambitious analysis, we use an automated software based on the MATISSE algorithm, originally designed for the GAIA/RVS spectral analysis. This software derives the atmospheric stellar parameters: effective temperature, surface gravity and the overall metallicity.Further improvements are foreseen in order to measure also individual abundances. By comparing the main physical and chemical properties of the host stars to those of the stellar population they belong to, this will bring new insights into the formation and evolution of exoplanetary systems and the star-planet connection.
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Moya, A. "Pulsating stars harbouring planets." EPJ Web of Conferences 47 (2013): 09005. http://dx.doi.org/10.1051/epjconf/20134709005.

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Dissertations / Theses on the topic "Stars with planets"

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Barker, Adrian John. "Tidal interactions between planets and stars." Thesis, University of Cambridge, 2011. https://www.repository.cam.ac.uk/handle/1810/240581.

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Since the first discovery of an extrasolar planet around a solar-type star, observers have detected over 500 planets outside the solar system. Many of these planets have Jovian masses and orbit their host stars in orbits of only a few days, the so-called 'Hot Jupiters'. At such close proximity to their parent stars, strong tidal interactions between the two bodies are expected to cause significant secular spin-orbit evolution. This thesis tackles two problems regarding the tidal evolution of short-period extrasolar planets. In the first part, we adopt a simple model of the orbit-averaged effects of tidal friction, to study the tidal evolution of planets on inclined orbits. We also analyse the effects of stellar magnetic braking. We then discuss the implications of our results for the importance of Rossiter-Mclaughlin effect observations. In the second part, we study the mechanisms of tidal dissipation in solar-type stars. In particular, internal gravity waves are launched at the interface of the convection and radiation zones of such a star, by the tidal forcing of a short-period planet. The fate of these waves as they approach the centre of the star is studied, primarily using numerical simulations, in both two and three dimensions. We find that the waves undergo instability and break above a critical amplitude. A model for the tidal dissipation that results from this process is presented, and its validity is verified by numerical integrations of the linear tidal response, in an extensive set of stellar models. The dissipation is efficient, and varies by less than an order of magnitude between all solar-type stars, throughout their main-sequence lifetimes, for a given planetary orbit. The implications of this mechanism for the survival of short-period extrasolar planets is discussed, and we propose a possible explanation for the survival of all of the extrasolar planets currently observed in short-period orbits around F, G and K stars. We then perform a stability analysis of a standing internal gravity wave near the centre of a solar-type star, to understand the early stages of the wave breaking process in more detail, and to determine whether the waves are subject to weaker parametric instabilities, below the critical amplitude required for wave breaking. We discuss the relevance of our results to our explanation for the survival of short-period planets presented in the second part of this thesis. Finally, we propose an alternative mechanism of tidal dissipation, involving the gradual radiative damping of the waves. Based on a simple estimate, it appears that this occurs even for low mass planets. However, it is in conflict with current observations since it would threaten the survival of all planets in orbits shorter than 2 days. We discuss some hydrodynamic instabilities and magnetic stresses which may prevent this process.
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Ortiz, Mauricio, Sabine Reffert, Trifon Trifonov, Andreas Quirrenbach, David S. Mitchell, Grzegorz Nowak, Esther Buenzli, et al. "Precise radial velocities of giant stars." EDP SCIENCES S A, 2016. http://hdl.handle.net/10150/622444.

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Context. For over 12 yr, we have carried out a precise radial velocity (RV) survey of a sample of 373 G- and K-giant stars using the Hamilton Echelle Spectrograph at the Lick Observatory. There are, among others, a number of multiple planetary systems in our sample as well as several planetary candidates in stellar binaries. Aims. We aim at detecting and characterizing substellar and stellar companions to the giant star HD 59686 A (HR 2877, HIP 36616). Methods. We obtained high-precision RV measurements of the star HD 59686 A. By fitting a Keplerian model to the periodic changes in the RVs, we can assess the nature of companions in the system. To distinguish between RV variations that are due to non-radial pulsation or stellar spots, we used infrared RVs taken with the CRIRES spectrograph at the Very Large Telescope. Additionally, to characterize the system in more detail, we obtained high-resolution images with LMIRCam at the Large Binocular Telescope. Results. We report the probable discovery of a giant planet with a mass of m(p) sin i = 6.92(-0.24)(+0.18) M-Jup orbiting at a(p) = 1.0860(-0.0007)(+0.0006) aufrom the giant star HD 59686 A. In addition to the planetary signal, we discovered an eccentric (e(B) = 0.729(-0.003)(+0.004)) binary companionwith a mass of m(B) sin i = 0.5296(-0.0008)(+0.0011) M-circle dot orbiting at a close separation from the giant primary with a semi-major axis of a(B) = 13.56(-0.14)(+0.18) au. Conclusions. The existence of the planet HD 59686 Ab in a tight eccentric binary system severely challenges standard giant planet formation theories and requires substantial improvements to such theories in tight binaries. Otherwise, alternative planet formation scenarios such as second-generation planets or dynamical interactions in an early phase of the system's lifetime need to be seriously considered to better understand the origin of this enigmatic planet.
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Daley-Yates, Simon. "Radio emission from hot stars and planets." Thesis, University of Birmingham, 2018. http://etheses.bham.ac.uk//id/eprint/8585/.

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The winds of hot massive stars and hot giant planets grant us insight into the mechanisms by which the interstellar medium is enriched and the history behind planetary system formation. This thesis comprises a series of studies investigating the magnetospheric dynamics and emission properties of both these astronomical bodies. An analytic study of thermal radio and sub-mm emission from the winds of massive stars investigates the contribution from acceleration and wind clumping. The results show strong variation of the spectral index, corresponding to the wind acceleration region and clumping of the wind. This shows a strong dependence of the emission on the wind velocity and clumping profile. By performing simulations of a magnetic rotating massive star with a non-zero dipole obliquity, it has been shown that the predicted radio and sub mm observable light curves and continuum spectra are highly dependent on the magnetic confinement of the stellar wind close to the surface, and that understanding the observer inclination and magnetic dipole obliquity are vital for determining the stellar mass-loss rate from radio observations. Hot Jupiter exoplanets are expected to produce strong radio emission in the MHz range but have not been detected. To explain the absence of observational results, simulations of the interactions between a solar type star and hot Jupiter were conducted and used to calculate the efficiency of radio emission generation within the planet's magnetosphere. Results show that it is completely inhibited by the planet's expanding atmosphere. Finally, the first simulations of wind-wind interactions between a solar type star and a short period hot Jupiter exoplanet that resolves accretion onto the surface of the star are presented. The accretion point, rate and periodicity are quantified, with the results indicating that material accreting onto the star perturbs surface density and temperature in a periodic manner, in agreement with observations.
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Jermyn, Adam Sean. "Turbulence and transport in stars and planets." Thesis, University of Cambridge, 2018. https://www.repository.cam.ac.uk/handle/1810/278021.

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In this dissertation I have argued that the study of stars and gaseous planets has relied too heavily on simplifying assumptions. In particular, I have demonstrated that the assumptions of spherical symmetry, thermal equilibrium, dynamical equilibrium and turbulent anisotropy all hide interesting phenomena which make a true difference to the structure and evolution of these bodies. To begin I developed new theoretical tools for probing these phenomena, starting with a new model of turbulent motion which accounts for many different sources of anisotropy. Building on this I studied rotating convection zones and determined scaling relations for the magnitude of differential rotation. In slowly-rotating systems the differential rotation is characterised by a power law with exponent of order unity, while in rapidly-rotating systems this exponent is strongly suppressed by the rotation. This provides a full characterisation of the magnitude of differential rotation in gaseous convection zones, and is in reasonable agreement with a wide array of simulations and observations. I then focused on the convection zones of rotating massive stars and found them to exhibit significantly anisotropic heat fluxes. This results in significant deviations from spherical symmetry and ultimately in qualitatively enhanced circulation currents in their envelopes. Accordingly, these stars ought to live much longer and have a different surface temperature. This potentially resolves several outstanding questions such as the anomalously slow evolution of stars on the giant branch, the dispersion in the observed properties of giant stars and the difficulty stellar modelling has to form massive binary black holes. In the same vein I examined the convection zones of bloated hot Jupiters and discovered a novel feedback mechanism between non-equilibrium tidal dissipation and the thermal structure of their upper envelopes. This mechanism stabilises shallow radiative zones against the convective instability, which would otherwise take over early on in the planet's formation as it proceeds to thermal equilibrium. Hence tidal dissipation is dramatically enhanced, which serves to inject significant quantities of heat into the upper layers of the planet and causes it to inflate. This mechanism can explain most of the observed population of inflated planets. Finally, I studied material mixing in the outer layers of accreting stars and developed a method for relating the observed surface chemistry to the bulk and accreting chemistries. This enables the direct inference of properties of circumstellar material and accretion rates for a wide variety of systems.
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Weldrake, David Thomas Fredrick, and weldrake@mpia-hd mpg de. "Giant Planets and Variable Stars in Globular Clusters." The Australian National University. Research School of Astronomy and Astrophysics, 2005. http://thesis.anu.edu.au./public/adt-ANU20050616.191315.

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Over the last decade, 135 extrasolar planets have been discovered, the vast majority found by ongoing radial velocity searches. Of the stars sampled in these searches, 1% have `Hot Jupiter' planets associated with them. Having masses equivalent to Jupiter yet orbital periods of only a few days, this new class of planet is clearly unlike anything in our Solar System.¶ Hot Jupiters present us with an intriguing prospect. If the orientation of the planetary orbit is close to edge-on, the planet will periodically transit across the face of its star, resulting in a small drop in brightness. This transit phenomenon has been successfully used for planet detection over the last couple of years, allowing determination of the planetary radius and accurate mass estimates when coupled with radial velocity observations.¶ To aid understanding of the effect stellar environment plays on Hot Jupiter formation and survivability, this thesis presents the results of a wide-field search for transiting Hot Jupiters in the globular cluster 47 Tucanae. This cluster presents many thousands of stars in a moderate field of view and provides the perfect target for a search of this nature. One previous transit search has been made in the central core of 47 Tuc; using the HST for 8.3 continuous days, Gilliland et.al (2000) expected 17 transits yet found none. This null result suggests that either system metallicity or stellar density may be inhibiting Hot Jupiter formation or survivability in the cluster.¶ This thesis presents a search for transits with a field of view 250 times larger than the HST search and samples the uncrowded outer halo of the cluster (previously unsampled for transits), providing important constraints on the effect of environment on Hot Jupiter formation. If planets are found, then stellar density would seem responsible for the Gilliland et.al (2000) core null result. If no planets are found to a significant level, the survey would provide strong evidence that system metallicity is the dominant factor. Using the ANU 40'' (1m) telescope at Siding Spring Observatory, a 30.4 night observing run was executed and photometry was derived via differential imaging. The dataset numbers 109,000 cluster (and field) stars for photometric analysis, of which 22,000 are suitable for the transit search. With a custom-written transit detection algorithm and extensive Monte Carlo simulations to model the dataset, seven planets should be detectable if the occurrence rate of Hot Jupiters is the same in the cluster as in the Solar Neighbourhood.¶ Despite a detailed search, no transit signatures were identified. This result strongly indicates that the low metallicity of the cluster is the dominant factor inhibiting planet formation in 47 Tuc. Current results in the Solar Neighbourhood show that planet frequency is strongly biased towards stars of high metallicity. This thesis shows that the metallicity trend is likely a universal phenomenon, not only limited to the immediate Solar Neighbourhood and raises questions of whether planets were much rarer in the earlier Universe.¶ As a side result of the search, 100 variable stars were identified in the field, 69 of which are new discoveries. Subsequent analysis reveals a strong period segregation among the cluster eclipsing binaries, indicating previously unobserved dynamical effects in the cluster. Distance estimates for both 47 Tuc and the SMC are in agreement with previously published values and an independent identification of the binary period-colour relation was observed. Two binaries seem to have low-luminosity companions worthy of followup and one variable is likely a star in the early phases of planetary nebula formation. All of the results presented in this thesis have been published in three separately refereed research papers.
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Weldrake, David Thomas Frederick. "Giant planets and variable stars in globular clusters /." View thesis entry in Australian Digital Theses Program, 2005. http://thesis.anu.edu.au/public/adt-ANU20050616.191315/index.html.

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Sainsbury-Martinez, Felix. "Flows, instabilities, and magnetism in stars and planets." Thesis, University of Exeter, 2017. http://hdl.handle.net/10871/32072.

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Flows, instabilities, and magnetism play significant roles in the internal and atmospheric dynamics of objects ranging from the smallest exoplanets to the largest stars. These phenomena are governed by the equations of magnetohydrodynamics (MHD), which link the flows and magnetic fields, and from which the operational parameters and growth rates of instabilities can be recovered. Here we present an overview of interesting phenomena (such as the internal dynamics of stellar and planetary objects, as well as instabilities which might operate within these environs), as well as computational techniques by which these phenomena might both be understood and analysed (through both ‘simplifications’ of the MHD equations and different numerical/computational approaches). We first present an investigation into the Heat-Flux-Driven Buoyancy Instability (HBI) within stellar and planetary atmospheres, considering both the parameter space it might operate within as well as its non-linear effects during said operation. We find that whilst the HBI may be able to play a role in Solar, stellar and planetary atmospheres, it is likely to be quite limited in scope, only operating within small regions. However, its dramatic consequences for heat transport in the non-linearly evolved state, and the prospects that it may operate outside the narrow regimes that our analytical analysis suggested, suggest that it may merit further study. This is followed with a discussion of a method by which the surface flows of exoplanets might be measured: The Rossiter-Mclaughlin Effect at Secondary Eclipse (RMse). We formulate the effect, showing that the formalism is identical to the traditional Rossiter-Mclaughlin effect, albeit in a different frame (a planet transiting a star becomes a star transiting a planet), and consider its observational implications: the effect should be observable for the brightest planet hosting stars using upcoming 40m-class telescopes (i.e.E-ELT). We finish with a series of 3D anelastic simulations of fully convective stars, designed to investigate how the internal flows are affected by varying stellar parameters, as well as a possible link between residual entropy and differential rotation contours, and a method by which this link can be used (via the thermal wind equation - TWE) to extrapolate the internal rotation. We find a clear transition between ‘solar-like’ and ‘anti-solar’ internal dynamics, characterised in the meridional circulation, differential rotation, residual entropy, and angular momentum flux profiles. Furthermore we find that, whilst the alignment between residual entropy and differential rotation contours is somewhat varied, the resultant extrapolation, via the TWE, produces a generally good fit to the differential rotation contours, suggesting a general robustness to the theory.
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Grether, Daniel Andrew Physics Faculty of Science UNSW. "Statistical analyses of extrasolar planets and other close companions to nearby stars." Awarded by:University of New South Wales. School of Physics, 2006. http://handle.unsw.edu.au/1959.4/29182.

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We analyse the properties of extrasolar planets, other close companions and their hosts. We start by identifying a sample of the detected extrasolar planets that is minimally affected by the selection effects of the Doppler detection method. With a simple analysis we quantify trends in the surface density of this sample in the Msini-period plane. A modest extrapolation of these trends puts Jupiter in the most densely occupied region of this parameter space, thus suggesting that Jupiter is a typical massive planet rather than an outlier. We then examine what fraction of Sun-like (~ FGK) stars have planets. We find that at least ~25% of stars possess planets when we limit our analysis to stars that have been monitored the longest and whose low surface activity allow the most precise radial velocity measurements. The true fraction of stars with planets may be as large as ~100%. We construct a sample of nearby Sun-like stars with close companions (period < 5 years). By using the same sample to extract the relative numbers of stellar, brown dwarf and planetary companions, we verify the existence of a very dry brown dwarf desert and describe it quantitatively. Approximately 16% of Sun-like stars have close companions more massive than Jupiter: 11% +- 3% are stellar, <1% are brown dwarf and 5% +- 2% are giant planets. A comparison with the initial mass function of individual stars and free-floating brown dwarfs, suggests either a different spectrum of gravitational fragmentation in the formation environment or post-formation migratory processes disinclined to leave brown dwarfs in close orbits. Finally we examine the relationship between the frequency of close companions and the metallicity of their Sun-like hosts. We confirm and quantify a ~4 sigma positive correlation between host metallicity and planetary companions. In contrast we find a ~2 sigma anti-correlation between host metallicity and the presence of a stellar companion. Upon dividing our sample into FG and K sub-samples, we find a negligible anti-correlation in the FG sub-sample and a ~3 sigma anti-correlation in the K sub-sample. A kinematic analysis suggests that this anti-correlation is produced by a combination of low-metallicity, high-binarity thick disk stars and higher-metallicity, lower-binarity thin disk stars.
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Petigura, Erik Ardeshir. "Prevalence of Earth-size Planets Orbiting Sun-like Stars." Thesis, University of California, Berkeley, 2015. http://pqdtopen.proquest.com/#viewpdf?dispub=3720767.

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In this thesis, I explore two topics in exoplanet science. The first is the prevalence of Earth-size planets in the Milky Way Galaxy. To determine the occurrence of planets having different sizes, orbital periods, and other properties, I conducted a survey of extrasolar planets using data collected by NASA’s Kepler Space Telescope. This project involved writing new algorithms to analyze Kepler data, finding planets, and conducting follow-up work using ground-based telescopes. I found that most stars have at least one planet at or within Earth’s orbit and that 26% of Sun-like stars have an Earth-size planet with an orbital period of 100 days or less.

The second topic is the connection between the properties of planets and their host stars. The precise characterization of exoplanet hosts helps to bring planet properties like mass, size, and equilibrium temperature into sharper focus and probes the physical processes that form planets. I studied the abundance of carbon and oxygen in over 1000 nearby stars using optical spectra taken by the California Planet Search. I found a large range in the relative abundance of carbon and oxygen in this sample, including a handful of carbon-rich stars. I also developed a new technique called SpecMatch for extracting fundamental stellar parameters from optical spectra. SpecMatch is particularly applicable to the relatively faint planet-hosting stars discovered by Kepler.

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Gallardo, José. "Physics of low mass stars, brown dwarfs and extrasolar planets." Lyon, École normale supérieure (sciences), 2007. http://www.theses.fr/2007ENSL0412.

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Books on the topic "Stars with planets"

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Mike, Goldsmith. Stars & planets. New York: Kingfisher, 2008.

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Channing, Margot. Stars & planets. Mankato, MN: Book House, 2015.

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Stars & planets. London: Dorling Kindersley, 2008.

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Borg, Janet. Stars & planets. New York: Lark Books, 2006.

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Watts, Claire. Stars & Planets. London: Dorling Kindersley Limited, 2008.

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1937-, Miner Ellis D., ed. Stars & planets. Lincolnwood, Ill: Publications International, 2007.

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Gregory, Bridges, ed. Stars & planets. [Alexandria, Va.]: Time-Life Books, 1996.

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Stars & planets. New York, N.Y: DK, 2007.

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Stars and planets. Victoria, Australia: Igloo Books, 2008.

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Ridpath, Ian. Stars and planets. Worthington, OH: Willowisp Press, 1985.

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Book chapters on the topic "Stars with planets"

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Reid, I. Neill, and Suzanne L. Hawley. "Extrasolar planets." In New Light on Dark Stars, 391–419. London: Springer London, 2000. http://dx.doi.org/10.1007/978-1-4471-3663-7_10.

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Barlow, Nadine G. "Terrestrial Planets." In Planets, Stars and Stellar Systems, 111–93. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5606-9_3.

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Wolszczan, A. "Planets Around Pulsars." In Compact Stars in Binaries, 187–96. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0167-4_15.

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Fischer, Daniel, and Hilmar Duerbeck. "Planets around Other Stars." In Hubble Revisited, 151–54. New York, NY: Springer New York, 1998. http://dx.doi.org/10.1007/978-1-4612-2232-3_22.

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Barbieri, Cesare. "Planets of Nearby Stars." In A Brief Introduction to the Search for Extra-Terrestrial Life, 97–104. Boca Raton, FL : CRC Press, Taylor & Francis Group, [2019]: CRC Press, 2019. http://dx.doi.org/10.1201/9780429201431-9.

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Hatzes, A. P., M. Döllinger, L. Pasquini, J. Setiawan, L. Girardi, and L. da Silva. "Planets Around Giant Stars." In Precision Spectroscopy in Astrophysics, 197–200. Berlin, Heidelberg: Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-75485-5_42.

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Setiawan, J., P. Weise, Th Henning, A. P. Hatzes, L. Pasquini, L. da Silva, L. Girardi, et al. "Planets Around Active Stars." In Precision Spectroscopy in Astrophysics, 201–4. Berlin, Heidelberg: Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-75485-5_43.

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Moya, A. "Pulsating Stars Harbouring Planets." In Astrophysics and Space Science Proceedings, 221–26. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-29630-7_41.

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Argyle, Bob, and R. W. Argyle. "Multiple Stars and Planets." In Observing and Measuring Visual Double Stars, 53–63. New York, NY: Springer New York, 2012. http://dx.doi.org/10.1007/978-1-4614-3945-5_5.

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Povh, Bogdan, and Mitja Rosina. "Stars, Planets, and Asteroids." In Scattering and Structures, 167–84. Berlin, Heidelberg: Springer Berlin Heidelberg, 2017. http://dx.doi.org/10.1007/978-3-662-54515-7_15.

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Conference papers on the topic "Stars with planets"

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Pilat-Lohinger, Elke, Zsolt Sándor, Markus Gyergyovits, and Ákos Bazsó. "Planets in Binary Stars." In Accretion Processes in Cosmic Sources – II. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.342.0010.

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Quirrenbach, Andreas, Sabine Reffert, and Christoph Bergmann. "Planets around Giant Stars." In PLANETARY SYSTEMS BEYOND THE MAIN SEQUENCE: Proceedings of the International Conference. AIP, 2011. http://dx.doi.org/10.1063/1.3556189.

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Geller, Aaron. "Dynamical Processing of Stars and Planets Through Star Clusters." In Frank N. Bash Symposium 2015. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.261.0006.

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Tanner, A., E. W. Geunther, E. Martin, M. R. Zapatero Osorio, and Eric Stempels. "Detecting Planets Around Low Mass Stars: The Gateway to Terrestrial 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/10.1063/1.3099104.

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Bear, Ealeal, and Noam Soker. "Planets around Extreme Horizontal Branch Stars." In PLANETARY SYSTEMS BEYOND THE MAIN SEQUENCE: Proceedings of the International Conference. AIP, 2011. http://dx.doi.org/10.1063/1.3556194.

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Rice, Ken, and Eric Stempels. "Building, moving and destroying 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/10.1063/1.3099147.

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Schultz, Alfred B., Daniel J. Schroeder, Ian J. Jordan, Fred Bruhweiler, Mike A. DiSanti, Helen M. Hart, Forrest C. Hamilton, et al. "Imaging planets about other stars with UMBRAS." In SPIE's International Symposium on Optical Science, Engineering, and Instrumentation, edited by Marija Strojnik and Bjorn F. Andresen. SPIE, 1999. http://dx.doi.org/10.1117/12.372685.

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Vlemmings, Wouter H. T. "Magnetic fields around evolved stars." In From Planets to Dark Energy: the Modern Radio Universe. Trieste, Italy: Sissa Medialab, 2008. http://dx.doi.org/10.22323/1.052.0070.

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Beichman, Charles A. "Terrestrial Planet Finder: the search for life-bearing planets around other stars." In Astronomical Telescopes & Instrumentation, edited by Robert D. Reasenberg. SPIE, 1998. http://dx.doi.org/10.1117/12.317137.

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Schultz, Alfred B., Ian J. Jordan, Helen M. Hart, Fred Bruhweiler, Dorothy A. Fraquelli, Forrest C. Hamilton, John L. Hershey, et al. "Imaging planets about other stars with UMBRAS II." In International Symposium on Optical Science and Technology, edited by Marija Strojnik and Bjorn F. Andresen. SPIE, 2000. http://dx.doi.org/10.1117/12.406562.

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Reports on the topic "Stars with planets"

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Hazi, A. Planets and Stars under the Magnifying Glass. Office of Scientific and Technical Information (OSTI), February 2007. http://dx.doi.org/10.2172/907853.

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Seidelmann, P. K., R. Gaume, N. Zacharias, K. J. Johnson, and B. Dorland. Optical Reference Stars for Space Surveillance: Future Plans: Latest Developments. Fort Belvoir, VA: Defense Technical Information Center, January 2010. http://dx.doi.org/10.21236/ada520456.

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Converse, Robert, Catherine W. McDonald, William Riddle, and Christine Youngblut. STARS (Software Technology for Adaptable and Reliable Systems) Methodology Area Summary. Volume 1. Organization and Plans. Fort Belvoir, VA: Defense Technical Information Center, March 1985. http://dx.doi.org/10.21236/ada163270.

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Worrell, Ernst, Tana Angelini, and Eric Masanet. Managing Your Energy: An ENERGY STAR(R) Guide for Identifying Energy Savings in Manufacturing Plants. Office of Scientific and Technical Information (OSTI), July 2010. http://dx.doi.org/10.2172/985911.

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Seidelmann, P. K., R. Gaume, N. Zacharias, K. Johnston, and B. Dorland. Optical Reference Star Catalogs for Space Surveillance: Current Status and Future Plans. Fort Belvoir, VA: Defense Technical Information Center, January 2007. http://dx.doi.org/10.21236/ada480193.

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Zilberman, Mark. Methods to Test the “Dimming Effect” Produced by a Decrease in the Number of Photons Received from Receding Light Sources. Intellectual Archive, November 2020. http://dx.doi.org/10.32370/iaj.2437.

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The hypothetical “Dimming Effect” describes the change of the number of photons arriving from a moving light source per unit of time. In non-relativistic systems, the “Dimming effect” may occur due to the growing distance of light sources moving away from the receiver. This means that due to the growing distance, the photons continuously require more time to reach the receiver, which reduces the number of received photons per time unit compared to the number of emitted photons. Understandably, the proposed “Dimming effect” must be tested (confirmed or rejected) through observations. a. This article provides the formula for the calculation of “Dimming effect” values using the redshift parameter Z widely used in astronomy. b. The “Dimming effect” can possibly be detected utilizing the orbital movement of the Earth around the Sun. In accordance to the “Dimming effect”, observers on Earth will view 1.0001 more photons per time unit emitted by stars located near the ecliptic plane in the direction of the Earth orbiting the Sun. And, in contrast, observers will view only 0.9999 photons per time unit emitted by stars located near the ecliptic plane in the direction opposite to the Earth orbiting the Sun. Calculating precise measurements of the same stars within a 6-month period can possibly detect this difference. These changes in brightness are not only for specific stars, as the change in brightness takes place for all stars near the ecliptic in the direction of the Earth’s orbit around the Sun and in the opposite direction. c. The “Dimming effect” can possibly be detected in a physics laboratory using a moving light source (or mirror) and photon counters located in the direction of travel and in the opposite direction. d. In theory, Dilation of time can also be used for testing the existence of the “Dimming effect.” However, in experiments on Earth this effect appears in only the 14th digit after the decimal point and testing does not appear to be feasible. e. Why is it important to test the “Dimming effect?” If confirmed, it would allow astronomers to adjust values of "Standard Candles" used in astronomy. Since “Standard Candles” are critical in various cosmological models, the “Dimming effect” can correct models and/or reveal and support new models. If it is proved that the “Dimming effect” does not exist, it will mean that the number of photons arriving per unit of time does not depend on the speed of the light source and observer, which is not so apparent.
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Eparkhina, Dina, Kieran Reilly, Michele Barbier, Elena Guista, Veronica Ortiz, Joaquin Tintore, and Nicole Köstner. Updated Dissemination and Exploitation Plan. EuroSea, October 2020. http://dx.doi.org/10.3289/eurosea_d8.2.

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Dissemination of project’s results and engagement with stakeholders towards a sustained results’ exploitation are intrinsically evolving. The vision of the project’s dissemination at the start of it should evolve as the activities progress. This plan presents an update on the EuroSea dissemination plans as seen a year after the kick-off.
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Figueroa, R. A., J. Carter, R. Rivera, and J. Otahal. Construction and start-up of a 250 kW natural gas fueled MCFC demonstration power plant. Office of Scientific and Technical Information (OSTI), December 1996. http://dx.doi.org/10.2172/460151.

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Motz, L. Lessons learned from an installation perspective for chemical demilitarization plant start-up at four operating incineration sites. Office of Scientific and Technical Information (OSTI), February 2011. http://dx.doi.org/10.2172/1006276.

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Galitsky, Christina, Ernst Worrell, and Christina Galitsky. Energy Efficiency Improvement and Cost Saving Opportunities for Cement Making. An ENERGY STAR Guide for Energy and Plant Managers. Office of Scientific and Technical Information (OSTI), January 2008. http://dx.doi.org/10.2172/927882.

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