Publications (187)434.19 Total impact

Article: Transiting exoplanets from the CoRoT space mission: XXIV. CoRoT24: A transiting multiplanet system
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ABSTRACT: We present the discovery of a candidate multiplytransiting system, the first one found in the CoRoT mission. Two transitlike features with periods of 5.11 and 11.76d are detected in the CoRoT light curve, around a main sequence K1V star of r=15.1. If the features are due to transiting planets around the same star, these would correspond to objects of 3.7$\pm$0.4 and 5.0$\pm$0.5 R_earth respectively. Several radial velocities serve to provide an upper limit of 5.7 M_earth for the 5.11~d signal, and to tentatively measure a mass of 28$^{+11}_{11}$ M_earth for the object transiting with a 11.76~d period. These measurements imply low density objects, with a significant gaseous envelope. The detailed analysis of the photometric and spectroscopic data serve to estimate the probability that the observations are caused by transiting Neptunesized planets as $>$26$\times$ higher than a blend scenario involving only one transiting planet, and $>$900$\times$ higher than a scenario involving two blends and no planets. The radial velocities show a long term modulation that might be attributed to a 1.5 M_jup planet orbiting at 1.8~A.U. from the host, but more data are required to determine the precise orbital parameters of this companion.06/2014;  [Show abstract] [Hide abstract]
ABSTRACT: We investigate the influence of impacts of large planetesimals and small planetary embryos on the early Martian surface on the hydrodynamic escape of an early steam atmosphere that is exposed to the high soft Xray and EUV flux of the young Sun. Impact statistics in terms of number, masses, velocities, and angles of asteroid impacts onto the early Mars are determined via nbody integrations. Based on these statistics, smoothed particle hydrodynamics (SPH) simulations result in estimates of energy transfer into the planetary surface material and according surface heating. For the estimation of the atmospheric escape rates we applied a soft Xray and EUV absorption model and a 1D upper atmosphere hydrodynamic model to a magma oceanrelated catastrophically outgassed steam atmosphere with surface pressure values of 52 bar H2O and 11 bar CO2. The estimated impact rates and energy deposition onto an early Martian surface can account for substantial heating. The energy influx and conversion rate into internal energy is most likely sufficient to keep a shallow magma ocean liquid for an extended period of time. Higher surface temperatures keep the outgassed steam atmosphere longer in vapor form and therefore enhance its escape to space within about 0.6 Myr after its formation.05/2014;  [Show abstract] [Hide abstract]
ABSTRACT: We take as dynamical model for extrasolar planetary systems a central star like our Sun and two giant planets m 1 and m 2 like Jupiter and Saturn. We change the mass ratio μ=m 2/m 1 of the two large planets for a wide range of 1/16 < μ < 16. We also change the ratio between the initial semimajor axes (ν=a 2/a 1) in the range of 1.2 < ν < 3 to model the different architecture of extrasolar planetary systems hosting two giant planets. The results for possible Trojans (Trojan planets) in the equilateral equilibrium points of the inner planet m 1 and the outer planet m 2 were derived with the aid of numerical integration. It turned out that in many configurations  depending on the mass ratios μ and the semimajor axes ratio ν  giant planets may host Trojans.03/2014;  [Show abstract] [Hide abstract]
ABSTRACT: We report the discovery of a massive and dense transiting planet CoRoT27b on a 3.58 day orbit around a 4.2 Gyrold G2~star. The planet candidate was identified from the CoRoT photometry, and was confirmed as a planet with groundbased spectroscopy. The confirmation of the planet candidate is based on radial velocity observations combined with imaging to rule out blends. The characterisation of the planet and its host star is carried out using a Bayesian approach where all the data (CoRoT photometry, radial velocities, and spectroscopic characterisation of the star) are used jointly. The Bayesian analysis includes a study whether the assumption of white normally distributed noise holds for the CoRoT photometry, and whether the use of a nonnormal noise distribution offers advantages in parameter estimation and model selection. CoRoT27b has a mass of $10.39 \pm 0.55$ $\mathrm{M}_{\rm Jup}$, a radius of $1.01 \pm 0.04$ $\mathrm{R}_{\rm Jup}$, a mean density of $12.6_{1.67}^{+1.92}$ $\mathrm{g\,cm^{3}}$, and an effective temperature of $1500 \pm 130$~K. The planet orbits around its host star, a 4.2 Gyrold G2star with a mass $M_{\star}=1.06$ $M_{\odot}$, and a radius $R_{\star}=1.05$ $R_{\odot}$, on a $0.048 \pm 0.007$ AU orbit every 3.58 days. The radial velocity observations allow us to exclude highly eccentric orbits, namely, $e<0.065$ with a 99% confidence. Given its high mass and density, theoretical modelling of CoRoT27b is demanding. We identify two solutions with heavy element mass fractions of $0.11\pm0.08$ $\mathrm{M_{\oplus}}$ and $0.07\pm0.06$ $\mathrm{M_{\oplus}}$, but even solutions void of heavy elements cannot be excluded. We carry out a secondary eclipse search from the CoRoT photometry using a method based on Bayesian model selection, but conclude that the noise level is too high to detect eclipses shallower than 9% of the transit depth.Astronomy and Astrophysics 02/2014; 562. · 5.08 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: Context. We investigate the effects of including material strength in multimaterial planetesimal collisions. Aims. The differences between strengthless material models and including the full elastoplastic model for solid bodies with brittle failure and fragmentation when treating collisions of asteroidsized bodies as they occur frequently in early planetary systems are demonstrated. Methods. We study impacts of bodies of Ceresmass with a solid rock target and an impactor with 30 wt% water content. The initial impact velocities and impact parameters are varied between the escape velocity $v_\mbox{esc}$ to about 6 $v_\mbox{esc}$ and from headon collisions to close flybys, respectively. We simulate the collisions using our own SPH code using both strengthless material and the full elastoplastic material model including brittle failure. Results. The qualitative analysis results in significant differences depending on whether material strength is included or not. This may be an effect of the relatively lowenergy impacts that cannot destroy the solid material instantly. One of the most prominent differences is the higher degree of fragmentation and shattered debris clouds in the solid case. As opposed to giant impacts we also observe some water ice to get transferred from the impactor to the target.12/2013;  [Show abstract] [Hide abstract]
ABSTRACT: We announce the discovery of 7 transiting planets around a Kepler target, a current record for transiting systems. Planets b, c, e and f are reported for the first time in this work. Planets d, g and h were previously reported in the literature (Batalha et al. 2013), although here we revise their orbital parameters and confirm their planetary nature. Planets h and g are gas giants and show strong dynamical interactions. The orbit of planet g is perturbed in such way that its orbital period changes by 25.7h between two consecutive transits during the length of the observations, which is the largest such perturbation found so far. The rest of the planets also show mutual interactions: planets d, e and f are superEarths close to a mean motion resonance chain (2:3:4), and planets b and c, with sizes below 2 Earth radii, are within 0.5% of the 4:5 mean motion resonance. This complex system presents some similarities to our Solar System, with small planets in inner orbits and gas giants in outer orbits. It is, however, more compact. The outer planet has an orbital distance around 1 AU, and the relative position of the gas giants is opposite to that of Jupiter and Saturn, which is closer to the expected result of planet formation theories. The dynamical interactions between planets are also much richer.The Astrophysical Journal 10/2013; 781(1). · 6.73 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: In this investigation we treat a special configuration of two celestial bodies in 1:1 mean motion resonance namely the socalled exchange orbits. There exist—at least—theoretically—two different types: the exchangea orbits and the exchangee orbits. The first one is the following: two celestial bodies are in orbit around a central body with almost the same semimajor axes on circular orbits. Because of the relatively small differences in semimajor axes they meet from time to time and exchange their semimajor axes. The inner one then moves outside the other planet and vice versa. The second configuration one is the following: two planets are moving on nearly the same orbit with respect to the semimajor axes, one on a circular orbit and the other one on an eccentric one. During their dynamical evolution they change the characteristics of the orbit, the circular one becomes an elliptic one whereas the elliptic one changes its shape to a circle. This ‘game’ repeats periodically. In this new study we extend the numerical computations for both of these exchange orbits to the three dimensional case and in another extension treat also the problem when these orbits are perturbed from a fourth body. Our results in form of graphs show quite well that for a large variety of initial conditions both configurations are stable and stay in these exchange orbits.Celestial Mechanics and Dynamical Astronomy 09/2013; · 2.32 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We investigate the distribution of encounter velocities and impact angles describing collisions in the habitable zone of the early planetary system. Here we present a catalogue of collision characteristics for a particular mass ratio of the colliding bodies and seven different planetesimal masses ranging from a tenth of Ceres' mass to 10 times the mass of the Moon. We show that there are virtually no collisions with impact speeds lower than the surface escape velocity and a similar velocityimpact angle distribution for different planetesimal masses if velocities are normalized using the escape velocity. An additional perturbing Jupiterlike object distorts the collision velocity and impact picture in the sense that grazing impacts at higher velocities are promoted if the perturber's orbit is close to the habitable zone whereas a more distant perturber has more the effect of a mere widening of the velocity dispersion.Proceedings of the International Astronomical Union 07/2013;  [Show abstract] [Hide abstract]
ABSTRACT: We give a brief introduction to smoothed particle hydrodynamics methods for continuum mechanics. Specifically, we present our 3D SPH code to simulate and analyze collisions of asteroids consisting of two types of material: basaltic rock and ice. We consider effects like brittle failure, fragmentation, and merging in different impact scenarios. After validating our code against previously published results we present first collision results based on measured values for the Weibull flaw distribution parameters of basalt.Astronomische Nachrichten 06/2013; · 1.40 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: The study of meteorite craters on Earth provides information about the dynamic evolution of bodies within the Solar System. Bosumtwi crater is a well studied, 10.5 km in diameter, ca. 1.07 Ma old impact structure located in Ghana. The impactor was �1 km in diameter, an ordinary chondrite and struck the Earth with an angle between 30� and 45� from the horizontal. We have used a two phase backward integration to constrain the most probable parent region of the impactor. We find that the most likely source region is a high inclination object from the Middle Main Belt.Astronomische Nachrichten 04/2013; 334(9):936. · 1.40 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: Investigations were carried out on the stability of the two gas giant system HD 60532 itself including additional, smaller bodies. The methods used were numerical simulations with the Lie Series integration method, and secular perturbation theory. The aims were to find stable regions for potential Earthlike planets within the system, and confirming the stability of the detected planets. As results, the given configuration can be considered stable for a period of at least 65 million years. The two planets create a large unstable section between 0.25 and 3.6 AU, where no additional body is able to remain stable. Variations in the mutual inclination between test bodies and the rest of the system of up to 20{\deg} have little effects on the size of the zone of instability.04/2013;  [Show abstract] [Hide abstract]
ABSTRACT: Hungaria asteroids, whose orbits occupy the region in element space between $1.78< a< 2.03$ AU, $e<0.19$, $12^\circ<i<31^\circ$, are a possible source of NearEarth Asteroids (NEAs). Named after (434) Hungaria these asteroids are relatively small, since the largest member of the group has a diameter of just about 11 km. They are mainly perturbed by Jupiter and Mars, possibly becoming Marscrossers and, later, they may even cross the orbits of Earth and Venus. In this paper we analyze the close encounters and possible impacts of escaped Hungarias with the terrestrial planets. Out of about 8000 known Hungarias we selected 200 objects which are on the edge of the group. We integrated their orbits over 100 million years in a simplified model of the planetary system (Mars to Saturn) subject only to gravitational forces. We picked out a sample of 11 objects (each with 50 clones) with large variations in semimajor axis and restarted the numerical integration in a gravitational model including the planets from Venus to Saturn. Due to close encounters, some of them achieve high inclinations and eccentricities which, in turn, lead to relatively high velocity impacts on Venus, Earth, and Mars. We statistically analyze all close encounters and impacts with the terrestrial planets and determine the encounter and impact velocities of these fictitious Hungarias.Planetary and Space Science 03/2013; 84(August 2013):513. · 2.11 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: The Hungaria asteroid family, which consists of more than 8000 members with semimajor axes between 1.78 and 2.03 AU, is regarded as one source for NearEarth Asteroids. Named after (434) Hungaria these asteroids are relatively small (mean diameter $\sim 1$ km) and have inclinations of the order of $20^\circ$. They are mainly perturbed by Jupiter and Mars, and are ejected because of mean motion and secular resonances with these planets and then become Marscrossers; later they may even cross the orbits of Earth and Venus. We are interested to analyse the close encounters and possible impacts with these planets. For 200 selected objects which are on the edge of the group we integrated their orbits over 100 million years in a simplified model of the planetary system (Mars to Saturn) subject to only gravitational forces. We picked out a sample of 11 objects (each with 50 clones) with large variations in semimajor axis and restarted the numerical integration in the model Venus to Saturn. Due to close encounters in connection with mean motion and secular resonances some of them achieve high inclinations and eccentricities which then leads to relatively high velocity impacts on Venus, Earth, and Mars. We report all close encounters and impacts with the terrestrial planets and statistically determine collision velocities of these fictitious Hungarias. With this data we compute the effect of the possible impacts with the terrestrial planets and estimate the diameter of the crater depending on the impact energy released, the impact velocity and the impact angle.10/2012;  åp. 05/2012; 541:A149.
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ABSTRACT: Recently the first Earth Trojan has been observed (Mainzer et al., ApJ 731) and found to be on an interesting orbit close to the Lagrange point L4 (Connors et al., Nature 475). In the present study we therefore perform a detailed investigation on the stability of its orbit and moreover extend the study to give an idea of the probability to find additional EarthTrojans. Our results are derived using different approaches: a) we derive an analytical mapping in the spatial elliptic restricted threebody problem to find the phase space structure of the dynamical problem. We explore the stability of the asteroid in the context of the phase space geometry, including the indirect influence of the additional planets of our Solar system. b) We use precise numerical methods to integrate the orbit forward and backward in time in different dynamical models. Based on a set of 400 clone orbits we derive the probability of capture and escape of the Earth Trojan asteroids 2010 TK7. c) To this end we perform an extensive numerical investigation of the stability region of the Earth's Lagrangian points. We present a detailed parameter study in the regime of possible stable tadpole and horseshoe orbits of additional EarthTrojans, i.e. with respect to the semimajor axes and inclinations of thousands of fictitious Trojans. All three approaches underline that the Earth Trojan asteroid 2010 TK7 finds himself in an unstable region on the edge of a stable zone; additional EarthTrojan asteroids may be found in this regime of stability.Astronomy and Astrophysics 02/2012; · 5.08 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: We report the discovery by the CoRoT space mission of a new giant planet, CoRoT20b. The planet has a mass of 4.24 ± 0.23 MJup and a radius of 0.84 ± 0.04 RJup. With a mean density of 8.87 ± 1.10 g cm3, it is among the most compact planets known so far. Evolutionary models for the planet suggest a mass of heavy elements of the order of 800 M⊕ if embedded in a central core, requiring a revision either of the planet formation models or both planet evolution and structure models. We note however that smaller amounts of heavy elements are expected by more realistic models in which they are mixed throughout the envelope. The planet orbits a Gtype star with an orbital period of 9.24 days and an eccentricity of 0.56.The star's projected rotational velocity is vsini = 4.5 ± 1.0 km s1, corresponding to a spin period of 11.5 ± 3.1 days if its axis of rotation is perpendicular to the orbital plane. In the framework of Darwinian theories and neglecting stellar magnetic breaking, we calculate the tidal evolution of the system and show that CoRoT20b is presently one of the very few Darwinstable planets that is evolving toward a triple synchronous state with equality of the orbital, planetary and stellar spin periods. The CoRoT space mission, launched on December 27th 2006, has been developed and is operated by CNES, with the contribution of Austria, Belgium, Brazil, ESA (RSSD and Science Programme), Germany, and Spain.Astronomy and Astrophysics 01/2012; 538:145. · 5.08 Impact Factor  Astronomy and Astrophysics. 01/2012; 237(20122):511529.
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ABSTRACT: As part of the national scientific network 'Pathways to Habitable Worlds' the delivery of water onto terrestrial planets is a key question since water is essential for the development of life as we know it. After summarizing the state of the art we show some first results of the transport of water in the early Solar System for scattered main belt objects. Hereby we investigate the questions whether planetesimals and planetesimal fragments which have gained considerable inclination due to the strong dynamical interactions in the main belt region around 2 AU can be efficient water transporting vessels. The Hungaria asteroid group is the best example that such scenarios are realistic. Assuming that the gas giants and the terrestrial planets are already formed, we monitor the collisions of scattered small bodies containing water (in the order of a few percent) with the terrestrial planets. Thus we are able to give a first estimate concerning the respective contribution of such bodies to the actual water content in the crust of the Earth.AIP Conference Proceedings 01/2012; 1468:137.  [Show abstract] [Hide abstract]
ABSTRACT: Observations of transiting extrasolar planets are of key importance to our understanding of planets because their mass, radius, and mass density can be determined. The CoRoT space mission allows us to achieve a very high photometric accuracy. By combining CoRoT data with highprecision radial velocity measurements, we derive precise planetary radii and masses. We report the discovery of CoRoT19b, a gasgiant planet transiting an old, inactive F9Vtype star with a period of four days. After excluding alternative physical configurations mimicking a planetary transit signal, we determine the radius and mass of the planet by combining CoRoT photometry with highresolution spectroscopy obtained with the echelle spectrographs SOPHIE, HARPS, FIES, and SANDIFORD. To improve the precision of its ephemeris and the epoch, we observed additional transits with the TRAPPIST and Euler telescopes. Using HARPS spectra obtained during the transit, we then determine the projected angle between the spin of the star and the orbit of the planet. We find that the host star of CoRoT19b is an inactive F9Vtype star close to the end of its mainsequence life. The host star has a mass M*=1.21+/0.05 Msun and radius R*=1.65+/0.04 Rsun. The planet has a mass of Mp=1.11+/0.06 Mjup and radius of Rp=1.29+/0.03 Rjup. The resulting bulk density is only rho=0.71+/0.06 gcm3, which is much lower than that for Jupiter. The exoplanet CoRoT19b is an example of a giant planet of almost the same mass as Jupiter but a 30% larger radius.åp. 12/2011; 537.  [Show abstract] [Hide abstract]
ABSTRACT: We report the detection of CoRoT23b, a hot Jupiter transiting in front of its host star with a period of 3.6314 \pm 0.0001 days. This planet was discovered thanks to photometric data secured with the CoRoT satellite, combined with spectroscopic radial velocity (RV) measurements. A photometric search for possible background eclipsing binaries conducted at CFHT and OGS concluded with a very low risk of false positives. The usual techniques of combining RV and transit data simultaneously were used to derive stellar and planetary parameters. The planet has a mass of Mp = 2.8 \pm 0.3 MJup, a radius of Rpl = 1.05 \pm 0.13 RJup, a density of \approx 3 g cm3. RV data also clearly reveal a non zero eccentricity of e = 0.16 \pm 0.02. The planet orbits a mature G0 main sequence star of V =15.5 mag, with a mass M\star = 1.14 \pm 0.08 M\odot, a radius R\star = 1. 61 \pm 0.18 R\odot and quasisolar abundances. The age of the system is evaluated to be 7 Gyr, not far from the transition to subgiant, in agreement with the rather large stellar radius. The two features of a significant eccentricity of the orbit and of a fairly high density are fairly uncommon for a hot Jupiter. The high density is, however, consistent with a model of contraction of a planet at this mass, given the age of the system. On the other hand, at such an age, circularization is expected to be completed. In fact, we show that for this planetary mass and orbital distance, any initial eccentricity should not totally vanish after 7 Gyr, as long as the tidal quality factor Qp is more than a few 105, a value that is the lower bound of the usually expected range. Even if Corot23b features a density and an eccentricity that are atypical of a hot Jupiter, it is thus not an enigmatic object.Astronomy and Astrophysics. 12/2011; 537(2012):A54.
Publication Stats
1k  Citations  
434.19  Total Impact Points  
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Institutions

1984–2014

University of Vienna
 Department of Astrophysics
Wien, Vienna, Austria


2012

Nanjing University
 Department of Astronomy
Nanching, Jiangsu Sheng, China


2010–2011

Instituto de Astrofísica de Canarias
San Cristóbal de La Laguna, Canary Islands, Spain


1999

University of Florida
 Department of Astronomy
Gainesville, FL, United States


1996

Athens State University
Athens, Alabama, United States


1993

Observatoire de la Côte d'Azur
Grasse, ProvenceAlpesCôte d'Azur, France
