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The Effects of Multiple Companions on the Efficiency of Space Interferometry Mission Planet Searches
The Space Interferometry Mission (SIM) is expected to make preciseastrometric measurements that can be used to detect low-mass planetsaround nearby stars. Since most nearby stars are members ofmultiple-star systems, many of them will have a measurable accelerationdue to their companion, which must be included when solving forastrometric parameters and searching for planetary perturbations. Inaddition, many of the stars with one radial velocity planet showindications of additional planets. Therefore, astrometric surveys suchas SIM must be capable of detecting planets and measuring orbitalparameters in systems with multiple stellar and/or planetary companions.We have conducted Monte Carlo simulations to investigate how thepresence of multiple companions affects the sensitivity of anastrometric survey such as SIM. We find that the detection efficiencyfor planets in wide binary systems is relatively unaffected by thepresence of a binary companion if the planetary orbital period is lessthan half the duration of the astrometric survey. For longer orbitalperiods, there are significant reductions in the sensitivity of anastrometric survey. In addition, we find that the signal required todetect a planet can be increased significantly due to the presence of anadditional planet orbiting the same star. Fortunately, adding a modestnumber of precision radial velocity observations significantly improvesthe sensitivity for many multiple-planet systems. Thus, the combinationof radial velocity observations and astrometric observations by SIM willbe particularly valuable for studying multiple-planet systems.
| The origin and chemical evolution of carbon in the Galactic thin and thick discs*
In order to trace the origin and evolution of carbon in the Galacticdisc, we have determined carbon abundances in 51 nearby F and G dwarfstars. The sample is divided into two kinematically distinct subsampleswith 35 and 16 stars that are representative of the Galactic thin andthick discs, respectively. The analysis is based on spectral synthesisof the forbidden [CI] line at 872.7nm using spectra of very highresolution (R~ 220000) and high signal-to-noise ratio (S/N >~ 300)that were obtained with the Coudé Echelle Spectrograph (CES)spectrograph by the European Southern Observatory (ESO) 3.6-m telescopeat La Silla in Chile. We find that [C/Fe] versus [Fe/H] trends for thethin and thick discs are totally merged and flat for subsolarmetallicities. The thin disc that extends to higher metallicities thanthe thick disc shows a shallow decline in [C/Fe] from [Fe/H]~ 0 and upto [Fe/H]~+0.4. The [C/O] versus [O/H] trends are well separated betweenthe two discs (due to differences in the oxygen abundances) and bear agreat resemblance to the [Fe/O] versus [O/H] trends. Our interpretationof our abundance trends is that the sources that are responsible for thecarbon enrichment in the Galactic thin and thick discs have operated ona time-scale very similar to those that are responsible for the Fe and Yenrichment [i.e. SNIa and asymptotic giant branch (AGB) stars,respectively]. We further note that there exist other observational datain the literature that favour massive stars as the main sources forcarbon. In order to match our carbon trends, we believe that the carbonyields from massive stars then must be very dependent on metallicity forthe C, Fe and Y trends to be so finely tuned in the two discpopulations. Such metallicity-dependent yields are no longer supportedby the new stellar models in the recent literature. For the Galaxy, wehence conclude that the carbon enrichment at metallicities typical ofthe disc is mainly due to low- and intermediate-mass stars, whilemassive stars are still the main carbon contributor at low metallicities(halo and metal-poor thick disc).
| Metallicity, debris discs and planets
We investigate the populations of main-sequence stars within 25 pc thathave debris discs and/or giant planets detected by Doppler shift. Themetallicity distribution of the debris sample is a very close match tothat of stars in general, but differs with >99 per cent confidencefrom the giant planet sample, which favours stars of above averagemetallicity. This result is not due to differences in age of the twosamples. The formation of debris-generating planetesimals at tens of authus appears independent of the metal fraction of the primordial disc,in contrast to the growth and migration history of giant planets withina few au. The data generally fit a core accumulation model, with outerplanetesimals forming eventually even from a disc low in solids, whileinner planets require fast core growth for gas to still be present tomake an atmosphere.
| Asteroseismology and interferometry .
Asteroseismology aims at constraining the stellar evolution theory, andallows to determine the age of stars together with other fundamentalparameters. We present recent results obtained by interferometry, andprospects for the future.
| Observing solar-like oscillations: recent results.
We review recent progress in observations of ground-based oscillations.Excellent observations now exist for a few stars (alpha Cen A{} and B,mu Ara), while there is some controversy over others (Procyon, etaBoo). We have reached the stage where single-site observations are oflimited value and where careful planning is needed to ensure the futureof asteroseismology.
| Stability and 2:1 resonance in the planetary system HD 829431
We have explored the secular dynamical evolution of the HD 82943 systemwith two resonant giant planets, by simulating various planetaryconfigurations via direct numerical integration. We also studied theirorbital motions in phase space. In the numerical integrations over107 yr, we found that all the stable orbits are connectedwith the 2:1 resonance. Typically, there exists the libration of the tworesonant arguments 1 and (or) 2 on the sametimescale. Hence, both of the semi-major axes are strongly constrainedto behave in a regular way, due to the confinement of the libration ofthe related angles. Using the analytical model we considered the motionof the inner planet in phase space for different values of the outerplanet's eccentricity e2 and of the relative apsidallongitude . We found that the 2:1 orbital resonance is easily preservedwhen= 0† and when e2 is not too large. A moderatee2 can lock the two planets into deep resonance. The resultsby the analytical method agree well with those by the numericalsimulation, both revealing the 2:1 resonance architecture.
| Spitzer IRS Spectroscopy of IRAS-discovered Debris Disks
We have obtained Spitzer Space Telescope Infrared Spectrograph (IRS)5.5-35 μm spectra of 59 main-sequence stars that possess IRAS 60μm excess. The spectra of five objects possess spectral features thatare well-modeled using micron-sized grains and silicates withcrystalline mass fractions 0%-80%, consistent with T Tauri and HerbigAeBe stars. With the exception of η Crv, these objects are youngwith ages <=50 Myr. Our fits require the presence of a cool blackbodycontinuum, Tgr=80-200 K, in addition to hot, amorphous, andcrystalline silicates, Tgr=290-600 K, suggesting thatmultiple parent body belts are present in some debris disks, analogousto the asteroid and Kuiper belts in our solar system. The spectra forthe majority of objects are featureless, suggesting that the emittinggrains probably have radii a>10 μm. We have modeled the excesscontinua using a continuous disk with a uniform surface densitydistribution, expected if Poynting-Robertson and stellar wind drag arethe dominant grain removal processes, and using a single-temperatureblackbody, expected if the dust is located in a narrow ring around thestar. The IRS spectra of many objects are better modeled with asingle-temperature blackbody, suggesting that the disks possess innerholes. The distribution of grain temperatures, based on our blackbodyfits, peaks at Tgr=110-120 K. Since the timescale for icesublimation of micron-sized grains with Tgr>110 K is afraction of a Myr, the lack of warmer material may be explained if thegrains are icy. If planets dynamically clear the central portions ofdebris disks, then the frequency of planets around other stars isprobably high. We estimate that the majority of debris disk systemspossess parent body masses, MPB<1 M⊕. Thelow inferred parent body masses suggest that planet formation is anefficient process.Based on observations with the NASA Spitzer Space Telescope, which isoperated by the California Institute of Technology for NASA.
| Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems
We present results of a reconnaissance for stellar companions to all 131radial velocity-detected candidate extrasolar planetary systems known asof 2005 July 1. Common proper-motion companions were investigated usingthe multiepoch STScI Digitized Sky Surveys and confirmed by matching thetrigonometric parallax distances of the primaries to companion distancesestimated photometrically. We also attempt to confirm or refutecompanions listed in the Washington Double Star Catalog, in the Catalogsof Nearby Stars Series by Gliese and Jahreiß, in Hipparcosresults, and in Duquennoy & Mayor's radial velocity survey. Ourfindings indicate that a lower limit of 30 (23%) of the 131 exoplanetsystems have stellar companions. We report new stellar companions to HD38529 and HD 188015 and a new candidate companion to HD 169830. Weconfirm many previously reported stellar companions, including six starsin five systems, that are recognized for the first time as companions toexoplanet hosts. We have found evidence that 20 entries in theWashington Double Star Catalog are not gravitationally bound companions.At least three (HD 178911, 16 Cyg B, and HD 219449), and possibly five(including HD 41004 and HD 38529), of the exoplanet systems reside intriple-star systems. Three exoplanet systems (GJ 86, HD 41004, andγ Cep) have potentially close-in stellar companions, with planetsat roughly Mercury-Mars distances from the host star and stellarcompanions at projected separations of ~20 AU, similar to the Sun-Uranusdistance. Finally, two of the exoplanet systems contain white dwarfcompanions. This comprehensive assessment of exoplanet systems indicatesthat solar systems are found in a variety of stellar multiplicityenvironments-singles, binaries, and triples-and that planets survive thepost-main-sequence evolution of companion stars.
| Catalog of Nearby Exoplanets
We present a catalog of nearby exoplanets. It contains the 172 knownlow-mass companions with orbits established through radial velocity andtransit measurements around stars within 200 pc. We include fivepreviously unpublished exoplanets orbiting the stars HD 11964, HD 66428,HD 99109, HD 107148, and HD 164922. We update orbits for 83 additionalexoplanets, including many whose orbits have not been revised sincetheir announcement, and include radial velocity time series from theLick, Keck, and Anglo-Australian Observatory planet searches. Both thesenew and previously published velocities are more precise here due toimprovements in our data reduction pipeline, which we applied toarchival spectra. We present a brief summary of the global properties ofthe known exoplanets, including their distributions of orbital semimajoraxis, minimum mass, and orbital eccentricity.Based on observations obtained at the W. M. Keck Observatory, which isoperated jointly by the University of California and the CaliforniaInstitute of Technology. The Keck Observatory was made possible by thegenerous financial support of the W. M. Keck Foundation.
| Orbital Configurations and Dynamical Stability of Multiplanet Systems around Sun-like Stars HD 202206, 14 Herculis, HD 37124, and HD 108874
We perform a dynamical analysis of the recently published radialvelocity (RV) measurements of a few solar-type stars that host multipleJupiter-like planets. In particular, we reanalyze the data for HD202206, 14 Her, HD 37124, and HD 108874. We derive dynamically stableconfigurations that reproduce the observed RV signals, using GAMP (thegenetic algorithm with MEGNO penalty). GAMP relies on N-body dynamicsand makes use of genetic algorithms merged with a stability criterion.For this purpose, we use the maximal Lyapunov exponent computed with thedynamical fast indicator MEGNO. Through a dynamical analysis of thephase space in a neighborhood of the obtained best-fit solutions, wederive meaningful limits on the parameters of the planets. Wedemonstrate that GAMP is especially well suited to the analysis of theRV data that only partially cover the longest orbital period and/or arerelated to multiplanet configurations involved in low-order mean motionresonances (MMRs). Our analysis reveals a presence of a secondJupiter-like planet in the 14 Her system (14 Her c) that is involved ina 3:1 or 6:1 MMR with the known companion 14 Her b. We also show thatthe dynamics of the HD 202206 system may be qualitatively different whencoplanar and mutually inclined orbits of the companions are considered.We demonstrate that the two outer planets in the HD 37124 system mayreside in a close neighborhood of the 5:2 MMR. Our results confirm thatthe HD 108874 system may be very close to a, or locked in an exact, 4:1MMR.
| Chemical Composition of the Planet-harboring Star TrES-1
We present a detailed chemical abundance analysis of the parent star ofthe transiting extrasolar planet TrES-1. Based on high-resolution KeckHIRES and Hobby-Eberly Telescope HRS spectra, we have determinedabundances relative to the Sun for 16 elements (Na, Mg, Al, Si, Ca, Sc,Ti, V, Cr, Mn, Co, Ni, Cu, Zn, Y, and Ba). The resulting averageabundance of <[X/H]>=-0.02+/-0.06 is in good agreement withinitial estimates of solar metallicity based on iron. We compare theelemental abundances of TrES-1 with those of the sample of stars withplanets, searching for possible chemical abundance anomalies. TrES-1appears not to be chemically peculiar in any measurable way. Weinvestigate possible signs of selective accretion of refractory elementsin TrES-1 and other stars with planets and find no statisticallysignificant trends of metallicity [X/H] with condensation temperatureTc. We use published abundances and kinematic information forthe sample of planet-hosting stars (including TrES-1) and severalstatistical indicators to provide an updated classification in terms oftheir likelihood to belong to either the thin disk or the thick disk ofthe Milky Way. TrES-1 is found to be very likely a member of thethin-disk population. By comparing α-element abundances of planethosts and a large control sample of field stars, we also find thatmetal-rich ([Fe/H]>~0.0) stars with planets appear to besystematically underabundant in [α/Fe] by ~0.1 dex with respect tocomparison field stars. The reason for this signature is unclear, butsystematic differences in the analysis procedures adopted by differentgroups cannot be ruled out.
| Bisectors of the cross-correlation function applied to stellar spectra. Discriminating stellar activity, oscillations and planets
Context: .Bisectors of strong, single spectral lines, usually the Fe I6252 line, have traditionally been used to examine the velocity fieldsin stellar atmospheres. This requires high S/N often achieved by summingmany individual spectra. Aims: .We investigate whether bisectorsderived from cross-correlation functions (CCF) of single-exposurespectra can be used to provide information on stellar atmospheres, andwhether they can be used to discriminate between radial velocity changescaused by planets, magnetic activity and oscillations. Methods:.Using a sample of bright stars observed with the HARPS spectrograph, weexamine the shapes of the bisectors of individual strong spectral linesin summed spectra, comparing with similar studies in the literature.Moreover, we examine four different quantitative CCF bisector measuresfor correlations with radial velocity and stellar parameters.Results: .We show that CCF bisector measures can be used forquantitative analysis, employing both the absolute values and thevariations. From absolute values, log g and absolute magnitude can beapproximated, and from the correlations with radial velocity one candistinguish between magnetic activity, oscillations and orbiting planetsas the probable cause of radial velocity variations. We confirm thatdifferent isolated spectral lines show different bisector shapes, evenbetween lines of the same element, calling for caution in trying toderive global stellar properties from the bisector of a CCF. For theactive star HR 1362 we suggest from the bisector shape an extraphotospheric heating caused by the chromosphere of several hundreddegrees. We confirm the fill-in of spectral lines of the Sun taken onthe daylight sky caused by Rayleigh-Brillouin and aerosol scattering,and we show for the first time that the fill-in has an asymmetriccomponent.
| A numerical study of the 2:1 planetary resonance
We numerically explore the long-term stability of planetary orbitslocked in a 2:1 mean motion resonance for a wide range of planetary massratios and orbital parameters. Our major tool is Laskar's frequency mapanalysis. Regions of low diffusion rate are outlined in a phase spacedefined by the two planetary eccentricities and the libration amplitudeof a critical resonance argument. Resonant systems that are dynamicallystable on a long timescale must lie within these regions. The resonancelocking between planets in high eccentric orbits may be destroyed bymutual close encounters. We discuss various dynamical protectionmechanisms related to the resonant configuration, among which is thewell-known apsidal corotation. In the case of moderate-to-loweccentricities, we find that apsidal circulators, little discussed tillnow, are very common among stable orbits. We also map the differenttypes of resonant behaviour predicted by analytical theories in thephase space.
| Birth and fate of hot-Neptune planets
This paper presents a consistent description of the formation and thesubsequent evolution of gaseous planets, with special attention toshort-period, low-mass hot-Neptune planets characteristic of μAra-like systems. We show that core accretion, including migration anddisk evolution, and subsequent evolution, taking irradiation andevaporation into account, provides a viable formation mechanism for thistype of strongly irradiated light planets. At an orbital distance a≃ 0.1 AU, this revised core accretion model leads to the formationof planets with total masses ranging from ~14 M⊕ (0.044M_J) to ~400 M⊕ (1.25 M_J). The newly born planets havea dense core of ~6 M⊕, independent of the total mass,and heavy element enrichments in the envelope, M_Z,env/M_env , varyingfrom 10% to 80% from the largest to the smallest planets. We examine thedependence of the evolution of the born planet on the evaporation ratedue to the incident XUV stellar flux. In order to reach a μ Ara-likemass (~14 M⊕) after 1 Gyr, the initial planetmass must range from 166 M⊕ (~0.52 M_J) to about 20M⊕, for evaporation rates varying by 2 orders ofmagnitude, which corresponds to 90% to 20% mass loss during evolution.The presence of a core and heavy elements in the envelope affects thestructure and the evolution of the planet appreciably and yields 8%-9% difference in radius compared to coreless objects of solarcomposition for Saturn-mass planets. These combinations of evaporationrates and internal compositions translate into different detectionprobabilities and thus into different statistical distributions forhot-Neptunes and hot-Jupiters. These calculations provide an observablediagnostic, namely a mass-radius-age relationship to distinguish betweenthe present core-accretion-evaporation model and the alternativecolliding core scenario for the formation of hot-Neptunes.
| About putative Neptune-like extrasolar planetary candidates
Context: .We re-analyze the precision radial velocity (RV) data of HD208487 by the Anglo-Australian Planet Search Team, HD 190360, HD 188015,HD 114729 by the California and Carnegie Planet Search Team, and HD147513 by the Geneva Planet Search Team. All these stars are supposed tohost Jovian companions in long-period orbits. Aims.We test a hypothesisthat the residuals of the 1-planet model of the RV or an irregularscatter of the measurements around the synthetic RV curve may beexplained by the existence of additional planets in short-period orbits.Methods. We performed a global search for the best fits in the orbitalparameters space with genetic algorithms and simplex method. This makesit possible to verify and extend the results with an application ofcommonly used FFT-based periodogram analysis for identifying the leadingperiods. Results. Our analysis confirms the presence of a periodiccomponent in the RV of HD 190360 that may correspond to a hot-Neptuneplanet. We found four new cases in which the 2-planet model yieldssignificantly better fits to the RV data than the best 1-planetsolutions. If the periodic variability of the residuals of single-planetfits indeed has a planetary origin, then hot-Neptune planets may existin these extrasolar systems. We estimate their orbital periods as in therange of 7-20 d and minimal masses of about 20 masses of the Earth.
| Abundances of refractory elements in the atmospheres of stars with extrasolar planets
Aims.This work presents a uniform and homogeneous study of chemicalabundances of refractory elements in 101 stars with and 93 without knownplanetary companions. We carry out an in-depth investigation of theabundances of Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Na, Mg and Al. The newcomparison sample, spanning the metallicity range -0.70< [Fe/H]<0.50, fills the gap that previously existed, mainly at highmetallicities, in the number of stars without known planets.Methods.Weused an enlarged set of data including new observations, especially forthe field "single" comparison stars . The line list previously studiedby other authors was improved: on average we analysed 90 spectral linesin every spectrum and carefully measured more than 16 600 equivalentwidths (EW) to calculate the abundances.Results.We investigate possibledifferences between the chemical abundances of the two groups of stars,both with and without planets. The results are globally comparable tothose obtained by other authors, and in most cases the abundance trendsof planet-host stars are very similar to those of the comparison sample.Conclusions.This work represents a step towards the comprehension ofrecently discovered planetary systems. These results could also beuseful for verifying galactic models at high metallicities andconsequently improve our knowledge of stellar nucleosynthesis andgalactic chemical evolution.
| Modeling β Virginis using seismological data
This paper presents the modeling of the F9 V star βVirginis based on seismological measurements. Using the Genevaevolution code including rotation and atomic diffusion, we find that twodistinct solutions reproduce all existing asteroseismic andnon-asteroseismic observational constraints well: a main-sequence modelwith a mass of 1.28 ± 0.03~Mȯ and an age t=3.24± 0.20 Gyr, or a model in the post-main sequence phase ofevolution with a lower mass of 1.21 ± 0.02~Mȯ andan age t=4.01 ± 0.30 Gyr. The small spacings δν02 and the ratio r02 between small and largespacings are sensitive to the differences in the structure of thecentral layers between these two solutions and are also sensitive to thestructural changes due to the rotational mixing. They can therefore beused to unambiguously determine the evolutionary state ofβ Vir and to study the effects of rotation onthe inner structure of the star. Unfortunately, existing asteroseismicdata do not enable such precise determination. We also show that thescatter in frequencies introduced by the rotational splittings canaccount for the larger dispersion of the observed large spacings for thenon-radial modes than for the radial modes.
| The HARPS search for southern extra-solar planets. V. A 14 Earth-masses planet orbiting HD 4308
We present here the discovery and characterisation of a very lightplanet around HD 4308. The planet orbits its star in 15.56 days. Thecircular radial-velocity variation presents a tiny semi-amplitude of 4.1m s-1 that corresponds to a planetary minimum mass m_2sin{i}= 14.1 Moplus (Earth masses). The planet was unveiled byhigh-precision radial-velocity measurements obtained with the HARPSspectrograph on the ESO 3.6-m telescope. The radial-velocity residualsaround the Keplerian solution are 1.3 m s-1, demonstratingthe very high quality of the HARPS measurements. Activity and bisectorindicators exclude any significant perturbations of stellar intrinsicorigin, which supports the planetary interpretation. Contrary to mostplanet-host stars, HD 4308 has a marked sub-solar metallicity ([Fe/H] =-0.31), raising the possibility that very light planet occurrence mightshow a different coupling with the parent star's metallicity than dogiant gaseous extra-solar planets. Together with Neptune-mass planetsclose to their parent stars, the new planet occupies a position in themass-separation parameter space that is constraining forplanet-formation and evolution theories. The question of whether theycan be considered as residuals of evaporated gaseous giant planets, icegiants, or super-earth planets is discussed in the context of the latestcore-accretion models.
| The Hunt for Extrasolar Planets at McDonald Observatory
Currently every major telescope at McDonald Observatory is utilized inthe search for extrasolar planets. We review the different planet searchefforts and present the results of these programs. In particular wedescribe in detail the on-going precise Doppler surveys at the Harlan J.Smith 2.7 m telescope and at the Hobby-Eberly Telescope (HET). Thehighlight of the HET program was last year's discovery of a "HotNeptune" in the ρ planetary system. With a mass of only 17 Earthmasses this object demonstrates our ability to detect extrasolar planetswith masses below the gas giant range.
| Astrophysics in 2004
In this 14th edition of ApXX,1 we bring you the Sun (§ 2) and Stars(§ 4), the Moon and Planets (§ 3), a truly binary pulsar(§ 5), a kinematic apology (§ 6), the whole universe(§§ 7 and 8), reconsideration of old settled (§ 9) andunsettled (§ 10) issues, and some things that happen only on Earth,some indeed only in these reviews (§§ 10 and 11).
| On the track of very low-mass planets with HARPS
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| A link between the semimajor axis of extrasolar gas giant planets and stellar metallicity
The fact that most extrasolar planets found to date are orbitingmetal-rich stars lends credence to the core accretion mechanism of gasgiant planet formation over its competitor, the disc instabilitymechanism. However, the core accretion mechanism is not refined to thepoint of explaining orbital parameters such as the unexpected semimajoraxes and eccentricities. We propose a model that correlates themetallicity of the host star with the original semimajor axis of itsmost massive planet, prior to migration, assuming that the coreaccretion scenario governs giant gas planet formation. The modelpredicts that the optimum regions for planetary formation shift inwardsas stellar metallicity decreases, providing an explanation for theobserved absence of long-period planets in metal-poor stars. We compareour predictions with the available data on extrasolar planets for starswith masses similar to the mass of the Sun. A fitting procedure producesan estimate of what we define as the zero-age planetary orbit (ZAPO)curve as a function of the metallicity of the star. The model hints thatthe lack of planets circling metal-poor stars may be partly caused by anenhanced destruction probability during the migration process, becausethe planets lie initially closer to their central star.
| Magnetospheric radio emission from extrasolar giant planets: the role of the host stars
We present a new analysis of the expected magnetospheric radio emissionfrom extrasolar giant planets (EGPs) for a distance limited sample ofthe nearest known extrasolar planets. Using recent results on thecorrelation between stellar X-ray flux and mass-loss rates from nearbystars, we estimate the expected mass-loss rates of the host stars ofextrasolar planets that lie within 20 pc of the Earth. We find that someof the host stars have mass-loss rates that are more than 100 times thatof the Sun and, given the expected dependence of the planetarymagnetospheric radio flux on stellar wind properties, this has a verysubstantial effect. Using these results and extrapolations of the likelymagnetic properties of the extrasolar planets, we infer their likelyradio properties.We compile a list of the most promising radio targets and conclude thatthe planets orbiting Tau Bootes, Gliese 86, Upsilon Andromeda and HD1237(as well as HD179949) are the most promising candidates, with expectedflux levels that should be detectable in the near future with upcomingtelescope arrays. The expected emission peak from these candidate radioemitting planets is typically ~40-50 MHz. We also discuss a range ofobservational considerations for detecting EGPs.
| Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs
We present a uniform catalog of stellar properties for 1040 nearby F, G,and K stars that have been observed by the Keck, Lick, and AAT planetsearch programs. Fitting observed echelle spectra with synthetic spectrayielded effective temperature, surface gravity, metallicity, projectedrotational velocity, and abundances of the elements Na, Si, Ti, Fe, andNi, for every star in the catalog. Combining V-band photometry andHipparcos parallaxes with a bolometric correction based on thespectroscopic results yielded stellar luminosity, radius, and mass.Interpolating Yonsei-Yale isochrones to the luminosity, effectivetemperature, metallicity, and α-element enhancement of each staryielded a theoretical mass, radius, gravity, and age range for moststars in the catalog. Automated tools provide uniform results and makeanalysis of such a large sample practical. Our analysis method differsfrom traditional abundance analyses in that we fit the observed spectrumdirectly, rather than trying to match equivalent widths, and wedetermine effective temperature and surface gravity from the spectrumitself, rather than adopting values based on measured photometry orparallax. As part of our analysis, we determined a new relationshipbetween macroturbulence and effective temperature on the main sequence.Detailed error analysis revealed small systematic offsets with respectto the Sun and spurious abundance trends as a function of effectivetemperature that would be inobvious in smaller samples. We attempted toremove these errors by applying empirical corrections, achieving aprecision per spectrum of 44 K in effective temperature, 0.03 dex inmetallicity, 0.06 dex in the logarithm of gravity, and 0.5 kms-1 in projected rotational velocity. Comparisons withprevious studies show only small discrepancies. Our spectroscopicallydetermined masses have a median fractional precision of 15%, but theyare systematically 10% higher than masses obtained by interpolatingisochrones. Our spectroscopic radii have a median fractional precisionof 3%. Our ages from isochrones have a precision that variesdramatically with location in the Hertzsprung-Russell diagram. We planto extend the catalog by applying our automated analysis technique toother large stellar samples.
| Five New Multicomponent Planetary Systems
We report Doppler measurements for six nearby G- and K-typemain-sequence stars that show multiple low-mass companions, at least oneof which has planetary mass. One system has three planets, the fourthtriple-planet system known around a normal star, and another has anextremely low minimum mass of 18 M⊕. HD 128311 (K0 V)has two planets (one previously known) with minimum masses (Msini) of2.18MJ and 3.21MJ and orbital periods of 1.26 and2.54 yr, suggesting a possible 2:1 resonance. For HD 108874 (G5 V), thevelocities reveal two planets (one previously known) having minimummasses and periods of (Msinib=1.36MJ,Pb=1.08 yr) and (Msinic=1.02MJ,Pc=4.4 yr). HD 50499 (G1 V) has a planet with P=6.8 yr andMsini=1.7MJ, and the velocity residuals exhibit a trend of-4.8 m s-1 yr-1, indicating a more distantcompanion with P>10 yr and minimum mass of 2MJ. HD 37124(G4 IV-V) has three planets, one having Msini=0.61MJ andP=154.5 days, as previously known. We find two plausible triple-planetmodels that fit the data, both having a second planet near P=840 days,with the more likely model having its third planet in a 6 yr orbit andthe other one in a 29 day orbit. For HD 190360, we confirm the planethaving P=7.9 yr and Msini=1.5MJ as found by the Geneva team,but we find a distinctly noncircular orbit with e=0.36+/-0.03, renderingthis not an analog of Jupiter as had been reported. Our velocities alsoreveal a second planet with P=17.1 days and Msini=18.1M⊕. HD 217107 (G8 IV) has a previously known ``hotJupiter'' with Msini=1.4MJ and P=7.13 days, and we confirmits high eccentricity, e=0.13. The velocity residuals reveal an outercompanion in an eccentric orbit, having minimum mass ofMsini>2MJ, eccentricity e~0.5, and a period P>8 yr,implying a semimajor axis a>4 AU and providing an opportunity fordirect detection. We have obtained high-precision photometry of five ofthe six planetary host stars with three of the automated telescopes atFairborn Observatory. We can rule out significant brightness variationsin phase with the radial velocities in most cases, thus supportingplanetary reflex motion as the cause of the velocity variations.Transits are ruled out to very shallow limits for HD 217107 and are alsoshown to be unlikely for the prospective inner planets of the HD 37124and HD 108874 systems. HD 128311 is photometrically variable with anamplitude of 0.03 mag and a period of 11.53 days, which is much shorterthan the orbital periods of its two planetary companions. This rotationperiod explains the origin of periodic velocity residuals to thetwo-planet model of this star. All of the planetary systems here wouldbe further constrained with astrometry by the Space InterferometryMission.Based on observations obtained at the W. M. Keck Observatory, which isoperated jointly by the University of California and the CaliforniaInstitute of Technology. Keck time has been granted by both NASA and theUniversity of California.
| Toward a Deterministic Model of Planetary Formation. III. Mass Distribution of Short-Period Planets around Stars of Various Masses
The origin of a recently discovered close-in Neptune-mass planet aroundGJ 436 poses a challenge to the current theories of planet formation. Onthe basis of the sequential accretion hypothesis and the standard theoryof gap formation and orbital migration, we show that around M dwarfstars, close-in Neptune-mass ice giant planets may be relatively common,while close-in Jupiter-mass gas giant planets are relatively rare. Themass distribution of close-in planets generally has two peaks at aboutNeptune mass and Jupiter mass. The lower mass peak takes the maximumfrequency for M dwarfs. Around more massive solar-type stars (G dwarfs),the higher mass peak is much more pronounced. Planets around G dwarfsundergo orbital migration after fully accreting gas, while those aroundM dwarfs tend to migrate before starting rapid gas accretion. Close-inNeptune-mass planets may also exist around G dwarfs, although they tendto be mostly composed of silicates and iron cores and their frequency isexpected to be much smaller than that of Neptune-mass planets around Mdwarfs and that of gas giants around G dwarfs. We also show that theconditions for planets' migration due to their tidal interaction withthe disk and the stellar mass dependence in the disk mass distributioncan be calibrated by the mass distribution of short-period planetsaround host stars with various masses.
| Single-Visit Photometric and Obscurational Completeness
We report a method that uses ``completeness'' to estimate the number ofextrasolar planets discovered by an observing program with adirect-imaging instrument. We develop a completeness function forEarth-like planets on ``habitable'' orbits for an instrument with acentral field obscuration, uniform sensitivity in an annular detectionzone, and limiting sensitivity that is expressed as a ``deltamagnitude'' with respect to the star, determined by systematic effects(given adequate exposure time). We demonstrate our method of estimationby applying it to our understanding of the coronagraphic version of theTerrestrial Planet Finder (TPF-C) mission as of 2004 October. Weestablish an initial relationship between the size, quality, andstability of the instrument's optics and its ability to meet missionscience requirements. We provide options for increasing the fidelity andversatility of the models on which our method is based, and we discusshow the method could be extended to model the TPF-C mission as a wholeto verify that its design can meet the science requirements.
| Three Low-Mass Planets from the Anglo-Australian Planet Search
We report the detection of three new low-mass planets from theAnglo-Australian Planet Search. The three parent stars of these planetsare chromospherically quiet main-sequence G dwarfs with metallicitiesranging from roughly solar (HD 117618 and HD 208487) to metal enriched(HD 102117). The orbital periods range from 20.8 to 130 days, theminimum masses from roughly 0.5MSat to 0.5MJup,and the eccentricities from 0.08 to 0.37, with the planet in thesmallest orbit (HD 102117) having the smallest eccentricity. Withsemiamplitudes of 10.6-19 m s-1, these planets induce Doppleramplitudes similar to those of Jupiter analogs, albeit with shorterperiods. Many of the most interesting future Doppler planets will bedetected at these semiamplitude levels, placing a premium on measurementprecision. The detection of such amplitudes in data extending back 6 yrgives confidence in the Anglo-Australian Planet Search's ability todetect Jupiter analogs as our time baseline extends to 12 yr. We discussthe criticality of such detections for the design of the next generationof extremely large telescopes and also highlight prospects for suitableobserving strategies to push to below 1 m s-1 precisions forbright stars in a search for sub-Neptunian planets.Based on observations obtained at the Anglo-Australian Telescope, SidingSpring, Australia.
| On the Period Distribution of Close-in Extrasolar Giant Planets
Transit (TR) surveys for extrasolar planets have recently uncovered apopulation of ``very hot Jupiters,'' planets with orbital periods ofP<=3 days. At first sight this may seem surprising, given that radialvelocity (RV) surveys have found a dearth of such planets, despite thefact that their sensitivity increases with decreasing P. We examine theconfrontation between RV and TR survey results, paying particularattention to selection biases that favor short-period planets in TRsurveys. We demonstrate that, when such biases and small-numberstatistics are properly taken into account, the period distributions ofplanets found by RV and TR surveys are consistent at better than the 1σ level. This consistency holds for a large range of reasonableassumptions. In other words, there are not enough planets detected torobustly conclude that the RV and TR short-period planet results areinconsistent. Assuming a logarithmic distribution of periods, we findthat the relative frequency of very hot Jupiters (VHJs; P=1-3 days) tohot Jupiters (HJs; P=3-9 days) is ~10%-20%. Given an absolute frequencyof HJs of ~1%, this implies that approximately one star in ~500-1000 hasa VHJ. We also note that VHJs and HJs appear to be distinct in terms oftheir upper mass limits. We discuss the implications of our results forplanetary migration theories as well as present and future TR and RVsurveys.
| Planets and Infrared Excesses: Preliminary Results from a Spitzer MIPS Survey of Solar-Type Stars
As part of a large Spitzer MIPS Guaranteed Time Observation program, wehave searched for infrared excesses due to debris disks toward 26 FGKfield stars known from radial velocity (RV) studies to have one or moreplanets. While none of these stars show excesses at 24 μm, we havedetected 70 μm excesses around six stars at the 3 σ confidencelevel. The excesses are produced by cool material (<100 K) locatedbeyond 10 AU, well outside the ``habitable zones'' of these systems andconsistent with the presence of Kuiper Belt analogs with ~100 times moreemitting surface area than in our own planetary system. Theseplanet-bearing stars are, by selection for RV studies, typically olderthan 1 Gyr, and the stars identified here with excesses have a medianage of 4 Gyr. We find a preliminary correlation of both the frequencyand the magnitude of dust emission with the presence of known planets.These are the first stars outside the solar system identified as havingboth well-confirmed planetary systems and well-confirmed IR excesses.
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Pozíciós és asztrometriai adatok
| Csillagkép: | Oltár |
| Rektaszcenzió: | 17h44m08.70s |
| Deklináció: | -51°50'03.0" |
| Vizuális fényesség: | 5.15 |
| Távolság: | 15.277 parszek |
| RA sajátmozgás: | -14.4 |
| Dec sajátmozgás: | -191.8 |
| B-T magnitude: | 5.964 |
| V-T magnitude: | 5.197 |
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