Contents
Images
Upload your image
DSS Images Other Images
Related articles
Changing stellar activity cycles
We investigated continuous long-term photometric datasets of thirteenactive stars, Ca II variability of one single main-sequence star, and10.7cm radio data of the Sun, with simple Fourier- and time-frequencyanalysis. The data reflect the strength of the activity manifested inmagnetic spots. All studied stars show multiple (2 to 4) cycles ofdifferent lengths. The time-frequency analysis reveals, that in severalcases of the sample one or two of the cycles exhibit continuous changes(increase or decrease). For four stars (V711 Tau, IL Hya, HK Lac, HD100180) and for the Sun we find that the cycle length changes arestrong, amounting to 10-50% during the observed time intervals. Thecycle lengths are generally longer for stars with longer rotationalperiods.
| Starspot activity in late stars: Methods and results
Three types of methods for studying the surface inhomogeneities of coolstars and the results of their use on type BY Dra, RS CVn, FK Com, and TTau variables are discussed. The current relevance of traditionalphotometric methods and the advantages of the zonal spottedness modelare pointed out. Dependences of the maximum total areas, averagelatitudes, and temperatures of spots on the global parameters of thestars are given. Analogs of the solar cycle in the variations of theareas and latitudes of starspots are examined, as well as the effects ofdifferential rotation and active longitudes.
| Mass loss and orbital period decrease in detached chromospherically active binaries
The secular evolution of the orbital angular momentum (OAM), thesystemic mass (M=M1+M2) and the orbital period of114 chromospherically active binaries (CABs) were investigated afterdetermining the kinematical ages of the subsamples which were setaccording to OAM bins. OAMs, systemic masses and orbital periods wereshown to be decreasing by the kinematical ages. The first-orderdecreasing rates of OAM, systemic mass and orbital period have beendetermined as per systemic OAM, per systemic mass and per orbitalperiod, respectively, from the kinematical ages. The ratio of d logJ/dlogM= 2.68, which were derived from the kinematics of the presentsample, implies that there must be a mechanism which amplifies theangular momentum loss (AML) times in comparison to isotropic AML ofhypothetical isotropic wind from the components. It has been shown thatsimple isotropic mass loss from the surface of a component or bothcomponents would increase the orbital period.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| On the Binary Nature of 1RXS J162848.1-415241
We present spectroscopy of the optical counterpart to 1RXSJ162848.1-41524, also known as the microquasar candidate MCQCJ162847-4152. All the data indicate that this X-ray source is not amicroquasar and that it is a single-lined chromospherically activebinary system with a likely orbital period of 4.9 days. Our analysissupports a K3 IV spectral classification for the star, which is dominantat optical wavelengths. The unseen binary component is most likely alate-type (K7-M) dwarf or a white dwarf. Using the high-resolutionspectra, we have measured the K3 star's rotational broadening to bevsini=43+/-3 km s-1 and determined a lower limit to thebinary mass ratio of q(=M2/M1)>2.0. The highrotational broadening together with the strong Ca II H and K/Hαemission and high-amplitude photometric variations indicate that theevolved star is very chromospherically active and responsible for theX-ray/radio emission.
| Mg II chromospheric radiative loss rates in cool active and quiet stars
The Mg II k emission line is a good indicator of the level ofchromospheric activity in late-type stars. We investigate the dependenceof this activity indicator on fundamental stellar parameters. To thispurpose we use IUE observations of the Mg II k line in 225 late-typestars of luminosity classes I-V, with different levels of chromosphericactivity. We first re-analyse the relation between Mg II k lineluminosity and stellar absolute magnitude, performing linear fits to thepoints. The ratio of Mg II surface flux to total surface flux is foundto be independent of stellar luminosity for evolved stars and toincrease with decreasing luminosity for dwarfs. We also analyse the MgII k line surface flux-metallicity connection. The Mg II k emissionlevel turns out to be not dependent on metallicity. Finally, the Mg II kline surface flux-temperature relation is investigated by treatingseparately, for the first time, a large sample of very active and normalstars. The stellar surface fluxes in the k line of normal stars arefound to be strongly dependent on the temperature and slightly dependenton the gravity, thus confirming the validity of recently proposedmodels. In contrast, data relative to RS CVn binaries and BY Dra stars,which show very strong chromospheric activity, are not justified in theframework of a description based only on acoustic waves and uniformlydistributed magnetic flux tubes so that they require more detailedmodels.
| Further Results of TiO-Band Observations of Starspots
We present measurements of starspot parameters (temperature and fillingfactor) on five highly active stars, using absorption bands of TiO, fromobservations made between 1998 March and 2001 December. We determinedstarspot parameters by fitting TiO bands using spectra of inactive G andK stars as proxies for the unspotted photospheres of the active starsand spectra of M stars as proxies for the spots. For three evolved RSCVn systems, we find spot filling factors between 0.28 and 0.42 for DMUMa, 0.22 and 0.40 for IN Vir, and 0.31 and 0.35 for XX Tri; thesevalues are similar to those found by other investigators usingphotometry and Doppler imaging. Among active dwarfs, we measured a lowerspot temperature (3350 K) for EQ Vir than found in a previous study ofTiO bands, and for EK Dra a lower spot temperature (~3800 K) than foundthrough photometry. For all active stars but XX Tri, we achieved goodphase coverage through a stellar rotational period. We also present ourfinal, extensive grid of spot and nonspot proxy stars.This paper includes data taken at McDonald Observatory of the Universityof Texas at Austin.
| The science case of the PEPSI high-resolution echelle spectrograph and polarimeter for the LBT
We lay out the scientific rationale for and present the instrumentalrequirements of a high-resolution adaptive-optics Echelle spectrographwith two full-Stokes polarimeters for the Large Binocular Telescope(LBT) in Arizona. Magnetic processes just like those seen on the Sun andin the space environment of the Earth are now well recognized in manyastrophysical areas. The application to other stars opened up a newfield of research that became widely known as the solar-stellarconnection. Late-type stars with convective envelopes are all affectedby magnetic processes which give rise to a rich variety of phenomena ontheir surface and are largely responsible for the heating of their outeratmospheres. Magnetic fields are likely to play a crucial role in theaccretion process of T-Tauri stars as well as in the acceleration andcollimation of jet-like flows in young stellar objects (YSOs). Anotherarea is the physics of active galactic nucleii (AGNs) , where themagnetic activity of the accreting black hole is now believed to beresponsible for most of the behavior of these objects, including theirX-ray spectrum, their notoriously dramatic variability, and the powerfulrelativistic jets they produce. Another is the physics of the centralengines of cosmic gamma-ray bursts, the most powerful explosions in theuniverse, for which the extreme apparent energy release are explainedthrough the collimation of the released energy by magnetic fields.Virtually all the physics of magnetic fields exploited in astrophysicsis somehow linked to our understanding of the Sun's and the star'smagnetic fields.
| The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of 14 000 F and G dwarfs
We present and discuss new determinations of metallicity, rotation, age,kinematics, and Galactic orbits for a complete, magnitude-limited, andkinematically unbiased sample of 16 682 nearby F and G dwarf stars. Our63 000 new, accurate radial-velocity observations for nearly 13 500stars allow identification of most of the binary stars in the sampleand, together with published uvbyβ photometry, Hipparcosparallaxes, Tycho-2 proper motions, and a few earlier radial velocities,complete the kinematic information for 14 139 stars. These high-qualityvelocity data are supplemented by effective temperatures andmetallicities newly derived from recent and/or revised calibrations. Theremaining stars either lack Hipparcos data or have fast rotation. Amajor effort has been devoted to the determination of new isochrone agesfor all stars for which this is possible. Particular attention has beengiven to a realistic treatment of statistical biases and errorestimates, as standard techniques tend to underestimate these effectsand introduce spurious features in the age distributions. Our ages agreewell with those by Edvardsson et al. (\cite{edv93}), despite severalastrophysical and computational improvements since then. We demonstrate,however, how strong observational and theoretical biases cause thedistribution of the observed ages to be very different from that of thetrue age distribution of the sample. Among the many basic relations ofthe Galactic disk that can be reinvestigated from the data presentedhere, we revisit the metallicity distribution of the G dwarfs and theage-metallicity, age-velocity, and metallicity-velocity relations of theSolar neighbourhood. Our first results confirm the lack of metal-poor Gdwarfs relative to closed-box model predictions (the ``G dwarfproblem''), the existence of radial metallicity gradients in the disk,the small change in mean metallicity of the thin disk since itsformation and the substantial scatter in metallicity at all ages, andthe continuing kinematic heating of the thin disk with an efficiencyconsistent with that expected for a combination of spiral arms and giantmolecular clouds. Distinct features in the distribution of the Vcomponent of the space motion are extended in age and metallicity,corresponding to the effects of stochastic spiral waves rather thanclassical moving groups, and may complicate the identification ofthick-disk stars from kinematic criteria. More advanced analyses of thisrich material will require careful simulations of the selection criteriafor the sample and the distribution of observational errors.Based on observations made with the Danish 1.5-m telescope at ESO, LaSilla, Chile, and with the Swiss 1-m telescope at Observatoire deHaute-Provence, France.Complete Tables 1 and 2 are only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/418/989
| Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution
The kinematics of 237 chromospherically active binaries (CABs) werestudied. The sample is heterogeneous with different orbits andphysically different components from F to M spectral-type main-sequencestars to G and K giants and supergiants. The computed U, V, W spacevelocities indicate that the sample is also heterogeneous in velocityspace. That is, both kinematically younger and older systems exist amongthe non-evolved main sequence and the evolved binaries containing giantsand subgiants. The kinematically young (0.95 Gyr) subsample (N= 95),which is formed according to the kinematical criteria of moving groups,was compared with the rest (N= 142) of the sample (3.86 Gyr) toinvestigate any observational clues of binary evolution. Comparing theorbital period histograms between the younger and older subsamples,evidence was found supporting the finding of Demircan that the CABs losemass (and angular momentum) and evolve towards shorter orbital periods.The evidence of mass loss is noticeable on the histograms of the totalmass (Mh+Mc), which is compared between theyounger (only N= 53 systems available) and older subsamples (only N= 66systems available). The orbital period decrease during binary evolutionis found to be clearly indicated by the kinematical ages of 6.69, 5.19and 3.02 Gyr which were found in the subsamples according to the periodranges of logP<= 0.8, 0.8 < logP<= 1.7 and 1.7 < logP<=3, respectively, among the binaries in the older subsample.
| Doppler imaging of stellar surface structure. XX. The rapidly-rotating single K2-giant HD 31993 = V1192 Orionis
We present two Doppler images from two consecutive stellar rotations ofthe single K2-giant HD 31993. Each Doppler image is reconstructed fromspectra obtained within a single stellar rotation. With its 25-dayrotational period and a radius of ~18 solar radii, HD 31993 isconsidered a very rapidly rotating star and thus allows the applicationof the Doppler-imaging technique, despite the unusually long period. Allmaps reveal 7 isolated, predominantly low-latitude spots with atemperature difference, photosphere minus spot, of just ~200 K. No polarspot or high-latitude activity above, say, +60° is seen. A largewarm feature is detected at high latitude and is believed to be real.These spots act as tracers for a cross correlation analysis and yield aclear signature of anti-solar differential surface rotation, i.e. thepolar regions rotating faster than the equator, with alpha =0.125+/-0.05 corresponding to a lap time of ~200 days. A detailed parameterstudy is carried out to verify the reality of the HD 31993 maps.
| A study of the Mg II 2796.34 Å emission line in late-type normal and RS CVn stars
We carry out an analysis of the Mg II 2796.34 Å emission line inRS CVn stars and make a comparison with the normal stars studied in aprevious paper (Paper I). The sample of RS CVn stars consists of 34objects with known HIPPARCOS parallaxes and observed at high resolutionwith IUE. We confirm that RS CVn stars tend to possess wider Mg II linesthan normal stars having the same absolute visual magnitude. However, wecould not find any correlation between the logarithmic line width logWdeg and the absolute visual magnitude MV (theWilson-Bappu relationship) for these active stars, contrary to the caseof normal stars addressed in Paper I. On the contrary, we find that astrong correlation exists in the (MV, log LMg II)plane (LMg II is the absolute flux in the line). In thisplane, normal and RS CVn stars are distributed along two nearly parallelstraight lines with RS CVn stars being systematically brighter by ~1dex. Such a diagram provides an interesting tool to discriminate activefrom normal stars. We finally analyse the distribution of RS CVn and ofnormal stars in the (log LMg II, log Wdeg) plane,and find a strong linear correlation for normal stars, which can be usedfor distance determinations.
| A Revised Calibration of the MV-W(O I 7774) Relationship using Hipparcos Data: Its Application to Cepheids and Evolved Stars
A new calibration of the MV-W(O I 7774) relationship hasbeen calculated using better reddening and distance estimates for asample of 27 calibrator stars of spectral types A to G, based onaccurate parallaxes and proper motions from the Hipparcos and Tychocatalogues. The present calibration predicts absolute magnitude withaccuracies of +/-0.38mag for a sample covering a large range ofMV, from -9.5 to +0.35 mag. The color term included in aprevious paper has been dropped since its inclusion does not lead to anysignificant improvement in the calibration. The variation of the O I7774 feature in the classical cepheid SS Sct has been studied. Wecalculated a phase-dependent correction to random phase OI featurestrengths in Cepheids, such that it predicts mean absolute magnitudesusing the above calibration. After applying such a correction, we couldincrease the list of calibrators to 58 by adding MV and O Itriplet strength data for 31 classical Cepheids. The standard error ofthe calibration using the composite sample was comparable to thatobtained from the primary 27 calibrators, showing that it is possible tocalculate mean Cepheid luminosities from random phase observations ofthe O I 7774 feature. We use our derived calibrations to estimateMV for a set of evolved objects to be able to locate theirpositions in the HR diagram.
| Hα variations of the RS CVn type binary ER Vulpeculae
We present the results of spectroscopic observations of the activeeclipsing binary ER Vul in the 5860-6700 Å spectral range carriedout at the Catania Astrophysical Observatory. Accurate measurements ofradial velocities by using the cross-correlation technique have beenmade and a new orbital solution is given. All spectra displaychromospheric emission which fills in the Hα absorption lines ofboth components. The equivalent width (EW) of the Hα emission hasbeen measured by subtraction of a synthetic spectrum built up withspectra of inactive standard stars. The EW of total Hα emission,arisen from both components, shows a phase-dependent variation. Itreaches its maximum value just before the primary eclipse. We were ableto separate the contributions to the Hα emission from theindividual components at phases far from the eclipses. We have foundthat the secondary, cooler component is the most active and its Hαresidual emission shows the same trend as the total Hα emission,along orbital phase. This Hα equivalent width variation can bedue to plage-like structures on the chromosphere of secondary star. Inaddition, a decrease of the Hα EW around the ingress phase of theprimary eclipse is apparent.
| Doppler imaging of stellar surface structure. XIX. The solar-type components of the close binary sigma2 Coronae Borealis
We present the first Doppler image for both stellar components of theF9+G0 ZAMS binary sigma 2 CrB and found evidence for thecoexistence of cool and warm spots on both stars. Cool spots appearmainly at polar or high latitudes while a confined equatorial warm beltappears on the trailing hemisphere of each of the two stars with respectto the orbital motion. We also present an update of the TempMap imagingcode that allows us to solve the stellar surface temperaturedistribution on both binary components simultaneously, includingphotometric input. Several test reconstructions are performed todemonstrate its reliability and robustness. Our new orbital solutionresults in very precise masses for both components - good to 0.4% - andconfirms the spectral classifications of F9 and G0 for the primary andsecondary, respectively. The visual component, sigma 1 CrB,seems to be G4 rather than G0. All three components are on or very closeto the ZAMS which is also confirmed by the relatively high lithiumabundance of about twenty times the solar abundance. Photometric lightvariations are detected with a period of 1.157+/- 0.002 days that weinterpret to be the rotation period of both binary components. A 0\fm04dimming in y together with a reddening of 0\fm01 in b-y during the year2000 suggests a long-term spot variability compatible with a period ofat least 260 days.
| Doppler images of starspots
I present a literature survey of the currently available Doppler imagesof cool stars. The 65 individual stars with Doppler images consist of 29single stars and 36 components in close binaries. Out of the total, 31were observed only once but 12 stars are (or were) being monitored foryears. Each image for each star is identified with the time when it wasobserved, whether photometry was used in the imaging, the inclination ofthe stellar rotation axis, the vsin i, the stellar rotation period, andwhether a polar spot and/or a high-latitude or low-latitude spot wasseen. The type of variable star and its M-K spectral classification isalso listed to identify the evolutionary status. The sample consists of3 classical T Tauri stars, 8 weak-lined T Tauri's, 27 main-sequencestars, 9 subgiants, and 18 giants. The total number of Doppler images is245 as of June 2002.
| Measuring starspots on magnetically active stars with the VLTI
We present feasibility studies to directly image stellar surfacefeatures, which are caused by magnetic activity, with the Very LargeTelescope Interferometer (VLTI). We concentrate on late typemagnetically active stars, for which the distribution of starspots onthe surface has been inferred from photometric and spectroscopic imaginganalysis. The study of the surface spot evolution during consecutiverotation cycles will allow first direct measurements (apart from theSun) of differential rotation which is the central ingredient ofmagnetic dynamo processes. The VLTI will provide baselines of up to 200m, and two scientific instruments for interferometric studies at near-and mid-infrared wavelengths. Imaging capabilities will be made possibleby closure-phase techniques. We conclude that a realistically modeledcool surface spot can be detected on stars with angular diametersexceeding ~ 2 mas using the VLTI with the first generation instrumentAMBER. The spot parameters can then be derived with reasonable accuracy.We discuss that the lack of knowledge of magnetically active stars ofthe required angular size, especially in the southern hemisphere, is acurrent limitation for VLTI observations of these surface features.
| Solar spots as prototypes for stellar spots
What is the nature of what we commonly refer to as starspots? The answerto that question determines what we can learn from the study ofstarspots about stars, their internal dynamics, and their magneticactivity. Observations of the Sun, the only cool star that we canobserve in detail, naturally led to the hypothesis that starspots inother cool stars are magneto-convective phenomena in which a magneticfield substantially affects the structure of a stellar atmosphere.Spectral line features, eclipse light curves, and intensity modulationsare consistent with that hypothesis. Yet for almost all stars for whichstarspots are reported, the surface coverage is very much higher thanfor the Sun, while many stars manifest spots at high latitudes where theSun has never been seen to do so. In this review, I address how wellstarspots compare to sunspots, discuss some differences expected whenmoving away from the Sun in the HR diagram or in level of activity, andidentify resources to further deepen our understanding.
| Hα spectroscopy and BV photometry of RT Lacertae
Contemporaneous spectroscopic and photometric B V observations of the RSCVn type eclipsing binary RT Lacertae were performedin summer 2000. The photometric observations were obtained at the EgeUniversity Observatory, while the spectroscopic ones were carried out atCatania Astrophysical Observatory in the spectral range 5860-6700Å. We obtained a high quality radial velocity curve of the systemthat allowed us to give more accurate values of the orbital parameters.A steady decrease of the barycentric velocity from 1920 to 2000 has beenpointed out and has been discussed in the context of a third bodyhypothesis. Through the subtraction of a ``synthetic'' spectrum, builtup with spectra of inactive standard stars, we detected Hα excessemission which fills in the photospheric absorption profiles of bothcomponents. With the exception of a few spectra, taken close to theeclipses, in which some extra absorption or a faint double-peaked broademission appears, there is no further evidence of circumstellar matterin this system, as suggested in previous works. The hotter and moremassive star appears also as the more active at a chromospheric level,since it has a Hα flux about ten times greater than the companion,on average. Rotational modulation of the Hα emission has beendetected in both stars. The hemisphere of the more massive star facingthe observer at phase 0fp75 appears brighter (in Hα ) than thatseen at phase 0fp25 , while for the less massive G9 IV star the maximumHα emission is seen around phase 0fp0-0fp1 . From the analysis ofthe contemporaneous light curve (Lanza et al. \cite{Lanza2001}), themore massive G5 IV star results to be more active than the companion ata photospheric level, in agreement with the chromospheric behaviourobserved in Hα . In addition, the starspots of the G5 IV star aremainly located in the Hα brighter hemisphere, suggesting a closespatial association of spots and plages in this star. The G9 IV stardisplays instead the maximum Hα emission at the phase of maximumvisibility of the smaller spotted area found from the light-curveanalysis. The minimum Hα emission occurs when the more heavilyspotted region is visible. Based on observations collected at CataniaAstrophysical Observatory, Italy, and at Ege University Observatory,Turkey. Table 1 only available at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/388/298
| New periodic variables from the Hipparcos epoch photometry
Two selection statistics are used to extract new candidate periodicvariables from the epoch photometry of the Hipparcos catalogue. Theprimary selection criterion is a signal-to-noise ratio. The dependenceof this statistic on the number of observations is calibrated usingabout 30000 randomly permuted Hipparcos data sets. A significance levelof 0.1 per cent is used to extract a first batch of candidate variables.The second criterion requires that the optimal frequency be unaffectedif the data are de-trended by low-order polynomials. We find 2675 newcandidate periodic variables, of which the majority (2082) are from theHipparcos`unsolved' variables. Potential problems with theinterpretation of the data (e.g. aliasing) are discussed.
| The Catania Automatic Photoelectric Telescope on Mt. Etna: a systematic study of magnetically active stars
A photometric monitoring of about 50 magnetically active stars, that arespread almost all over the H-R diagram, was initiated at the mountainstation of Catania Observatory on Mt. Etna (1750-m a.s.l.) in 1992 withan 80-cm robotic telescope (APT-80) built by AutoScope Co. (USA). Thissystematic survey is now approaching its 10th year anniversary. For mostof the stars, quite well defined solar-like spot maps have been derivedfrom UBV data obtained in different epochs. These data have allowed usto investigate some relevant characteristics of spot activity andvariability on stars, and to obtain clear evidence of long-term activitycycles, in the range from a few to about 10 years, on some of theobserved targets. Starspot maps are constructed by using advanced tools,such as massive parallel computing and are based on Maximum Entropy andTikhonov regularization criteria. Selected results are here presented.Our systematic observation program is still underway and a secondAPT80/2, equipped with a CCD camera, will pair the APT80/1 on the samesite. Its operation is foreseen for mid 2002.
| BVR photometry and Hα spectroscopy of RS CVn type binary MM Herculis
The RS CVn type eclipsing binary MM Herculis wasobserved photo-electrically using B, V and R filters in 1998 and 1999and the light and colour curves were obtained. Spectroscopicobservations were carried out in 1999. The new light and colour curvesare anti-correlated with the observations of 1997, i.e. the system isbluer when it is faintest. The variations of the brightnesses at eachspecial phase (0.0, 0.25, 0.5, and 0.75) show an almost cyclic changewith a period of about 6 years. This value is in good agreement with themigration periods of the spots suggested by us previously. Theoutside-of-eclipse wave in the light curve shows a minimum at phase~0.50, and the mean colour of the system is the bluest at the samephase. When the spots located on the cooler component are seen aroundphase 0.50, the amplitude of the light variation outside eclipse islarger than the others. Such variation may be caused by the effect ofthe hotter component. Spectroscopic observations of the system werecarried out in the spectral range 5860-6700 Å. The subtraction ofa ``synthetic'' spectrum, built up with spectra of inactive standardstars, allows us to detect an Hα emission excess only from thecool component. New radial velocity measurements of the system wereobtained and analyzed for the orbital parameters. Based on observationscollected at the Ege University Observatory, Turkey, and at the CataniaAstrophysical Observatory, Italy.
| Doppler imaging of stellar surface structure. XVI. A time-series analysis of the moderately-rotating K1-giant sigma Geminorum
We present a simultaneous photometric and spectroscopic imaging analysisof the long-period RS CVn binary sigma Gem, covering 3.6 consecutiverotation cycles with high time resolution. From six overlapping butconsecutive Doppler maps we trace the evolution of individual spotsthroughout the time range covered. All spots group either along a bandat approximately +45 degrees latitude and a width of 30 degrees, orappear centered at the equator. No polar spot is detected. We did notfind a conclusive migration pattern from the cross-correlation maps fromone rotation to the next and attribute this to a masking effect ofshort-term spot changes.
| Stars with the Largest Hipparcos Photometric Amplitudes
A list of the 2027 stars that have the largest photometric amplitudes inHipparcos Photometry shows that most variable stars are all Miras. Thepercentage of variable types change as a function of amplitude. Thiscompilation should also be of value to photometrists looking forrelatively unstudied, but large amplitude stars.
| Doppler imaging from artificial data. Testing the temperature inversion from spectral-line profiles
We present extensive numerical tests of our temperature-based imagereconstruction code TempMap. Two test cases that represent arapidly-rotating low-inclination star and a moderately-rotatinghigh-inclination star are used for the forward problem. Tests are thenmade to recover the original input map and include data errors andinput-parameter errors. The former include variations of photon noise,continuum displacement, continuum slopes, scattered light in thespectrograph, and phase gaps with and without continuum information. Theinput-parameter tests include the confusion in the recovery of hotversus cool spots, uncertainties of atmospheric parameters such asradial-tangential macroturbulence and gravity, and the influence of linestrength and line damping. In general, we find that the geometricinformation is less dependent on photon noise and on input errors thanthe temperature information. Our test inversions also show that, at thevsin i of these test cases, no significant gain in image quality isachieved once S/N of 300:1 is surpassed.
| Doppler imaging of stellar surface structure --- XIV. The double-lined pre-main-sequence binary V 824 Arae = HD 155555
Photospheric Doppler images for both stellar components of thedouble-lined pre-main-sequence binary V 824 Ara reveal surfacetemperature inhomogeneities of up to 1800 K on both stars. The spotgeometry on the hotter primary is dominated by an elongated, tilted,equatorial feature but our maps from two spectral regions consistentlyalso show a polar spot cooler by 1700 K. The secondary star has spotsmainly at low and very high latitudes but not a full-sized polar cap. Aflux-tube simulation with appropriate stellar models for V 824 Arasuggests that any polar or high-latitude spot must have formed afterflux-tube emergence. Generally, the low-latitude spots on both stellarcomponents appear to be mostly concentrated on the hemispheres turnedaway from each other while the asymmetry of the polar spot on theprimary points in the direction of the orbital motion. We present newradial velocities and use them to re- evaluate the orbital elements andto derive absolute parameters for both stellar components. The absolutebrightness and mass of the two stars suggest that they are very close tothe main sequence - but not yet on the ZAMS - if an inclination of theorbital plane (and rotational axes) of 52̂ is adopted as suggestedby the Doppler imaging. Since both stars are active, we solve for theinclinations of both stellar components separately and find that thevalues agree to within their uncertainties. Based on observationscollected at the European Southern Observatory
| The long-period RS CVn binary IM Pegasi --- II. First surface images
New high-resolution, high signal-to-noise ratio spectroscopicobservations and UBV photometry carried out in 1996-1999 were analysedwith the surface imaging technique. A total of 8 images of IM Peg wasobtained for the first time. A huge high-latitude active region wasfound to dominate the stellar surface and decreased in area during theperiod of the observations. At the same time, on the opposite hemisphere(in longitudes), smaller spots were developing. The spots were migratingin the orbital reference frame, the period of spot rotation being of24.d73∓0.d02. The spots constitute two active longitudes onopposite stellar hemispheres, similar to other RS CVn stars. Theevolution of the spot areas within the active longitudes indicates astellar activity cycle, during which one active longitude dominates thestellar activity, to be about 6.5 years. Then, a total cycle, comprisingtwo consecutive periods of activity of both active longitudes, is about13 years. In 1999, the activity switched to the other active longitude.This declared the beginning of a new (half-) cycle. based onobservations collected at the Nordic Optical Telescope (NOT), La Palma,Spain; the 2.6 m and 1.25 m telescopes of the Crimean AstrophysicalObservatory, Ukraine; the 2m telescope of the National AstronomicalObservatory, Rozhen, Bulgaria.
| Astrophysics in 1999
The year 1999 saw the arrival of a star with three planets, a universewith three parameters, and a solar corona that could be heated at leastthree ways. In addition, there were at least three papers on everyquestion that has ever been asked in astrophysics, from ``Will theUniverse expand forever?'' to ``Does mantle convection occur in one ortwo layers?'' The answers generally were, ``Yes,'' ``No,'' and ``None ofthe above,'' to each of the questions. The authors have done their bestto organize the richness around centers defined by objects, methods, andmadnesses.
| Photometric Measurements of the Fields of More than 700 Nearby Stars
In preparation for optical/IR interferometric searches for substellarcompanions of nearby stars, we undertook to characterize the fields ofall nearby stars visible from the Northern Hemisphere to determinesuitable companions for interferometric phase referencing. Because theKeck Interferometer in particular will be able to phase-reference oncompanions within the isoplanatic patch (30") to about 17th magnitude atK, we took images at V, r, and i that were deep enough to determine iffield stars were present to this magnitude around nearby stars using aspot-coated CCD. We report on 733 fields containing 10,629 measurementsin up to three filters (Gunn i, r and Johnson V) of nearby stars down toabout 13th magnitude at V.
| Starspot photometry with robotic telescopes. UBV(RI)_C and by light curves of 47 active stars in 1996/97
We present continuous multicolor photometry for 47 stars from October1996 through June 1997. Altogether, 7073 V(RI)_c, UBV, and by datapoints, each the average of three individual readings, were acquiredwith three automatic photoelectric telescopes (APTs) at FairbornObservatory in southern Arizona. Most of our targets arechromospherically active single and binary stars of spectral type G to Kbut there are also four pre-main-sequence objects and three pulsatingstars in our sample. The light variability is generally due torotational modulation of an asymmetrically spotted stellar surface andtherefore precise rotational periods and their seasonal variations aredetermined from Fourier analysis. We also report on photometricvariations of gamma CrB (A0V) with a period of 0.44534 days. All dataare available in numerical form. All data are available from CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
|
Submit a new article
Related links
Submit a new link
Member of following groups:
|
Observation and Astrometry data
| Constellation: | さんかく座 |
| Right ascension: | 02h03m47.12s |
| Declination: | +35°35'28.7" |
| Apparent magnitude: | 8.428 |
| Distance: | 196.85 parsecs |
| Proper motion RA: | -51.6 |
| Proper motion Dec: | -13.6 |
| B-T magnitude: | 9.832 |
| V-T magnitude: | 8.544 |
Catalogs and designations:
|
INHABITED SKY
