תוכן
תמונות
הוסף תמונה שלך
DSS Images Other Images
מאמרים קשורים
Hubble Space Telescope Optical Imaging of the Eroding Debris Disk HD 61005
We present Hubble Space Telescope optical coronagraphic polarizationimaging observations of the dusty debris disk HD 61005. The scatteredlight intensity image and polarization structure reveal a highlyinclined disk with a clear asymmetric, swept back component, suggestiveof significant interaction with the ambient interstellar medium (ISM).The combination of our new data with the published 1.1 ?m discoveryimage shows that the grains are blue scattering with no strong colorgradient as a function of radius, implying predominantly submicron-sizedgrains. We investigate possible explanations that could account for theobserved swept back, asymmetric morphology. Previous work has suggestedthat HD 61005 may be interacting with a cold, unusually denseinterstellar cloud. However, limits on the intervening interstellar gascolumn density from an optical spectrum of HD 61005 in the Na I D linesrender this possibility unlikely. Instead, HD 61005 may be embedded in amore typical warm, low-density cloud that introduces secularperturbations to dust grain orbits. This mechanism can significantlydistort the ensemble disk structure within a typical cloud crossingtime. For a counterintuitive relative flow direction—parallel tothe disk midplane—we find that the structures generated by thesedistortions can very roughly approximate the HD 61005 morphology. Futureobservational studies constraining the direction of the relative ISMflow will thus provide an important constraint for future modeling.Independent of the interpretation for HD 61005, we expect thatinterstellar gas drag likely plays a role in producing asymmetriesobserved in other debris disk systems, such as HD 15115 and ?Velorum.
| Effective temperature scale and bolometric corrections from 2MASS photometry
We present a method to determine effective temperatures, angularsemi-diameters and bolometric corrections for population I and II FGKtype stars based on V and 2MASS IR photometry. Accurate calibration isaccomplished by using a sample of solar analogues, whose averagetemperature is assumed to be equal to the solar effective temperature of5777 K. By taking into account all possible sources of error we estimateassociated uncertainties to better than 1% in effective temperature andin the range 1.0-2.5% in angular semi-diameter for unreddened stars.Comparison of our new temperatures with other determinations extractedfrom the literature indicates, in general, remarkably good agreement.These results suggest that the effective temperaure scale of FGK starsis currently established with an accuracy better than 0.5%-1%. Theapplication of the method to a sample of 10 999 dwarfs in the Hipparcoscatalogue allows us to define temperature and bolometric correction (Kband) calibrations as a function of (V-K), [m/H] and log g. Bolometriccorrections in the V and K bands as a function of T_eff, [m/H] and log gare also given. We provide effective temperatures, angularsemi-diameters, radii and bolometric corrections in the V and K bandsfor the 10 999 FGK stars in our sample with the correspondinguncertainties.
| Mining the Metal-rich Stars for Planets
We examine the correlation between stellar metallicity and the presenceof short-period planets. It appears that approximately 1% of dwarf starsin the solar neighborhood harbor short-period planets characterized bynear-circular orbits and orbital periods P<20 days. However, amongthe most metal-rich stars (defined as having [Fe/H]>0.2 dex), itappears that the fraction increases to 10%. Using the Hipparcos databaseand the Hauck & Mermilliod compilation of Strömgren uvbyphotometry, we identify a sample of 206 metal-rich stars of spectraltype K, G and F which have an enhanced probability of harboringshort-period planets. Many of these stars would be excellent candidatesfor addition to radial velocity surveys. We have searched the Hipparcosepoch photometry for transiting planets within our 206 star catalog. Wefind that the quality of the Hipparcos data is not high enough to permitunambiguous transit detections. It is, however, possible to identifycandidate transit periods. We then discuss various ramifications of thestellar metallicity-planet connection. First, we show that there ispreliminary evidence for increasing metallicity with increasing stellarmass among known planet-bearing stars. This trend can be explained by ascenario in which planet-bearing stars accrete an average of 30M⊕ of rocky material after the gaseous protoplanetarydisk phase has ended. We present dynamical calculations which suggestthat a survey of metallicities of spectroscopic binary stars can be usedto understand the root cause of the stellar metallicity-planetconnection.
| SANTIAGO 91, a right ascension catalogue of 3387 stars (equinox J2000).
The positions in right ascension of 3387 stars belonging to the Santiago67 Catalogue, observed with the Repsold Meridian Circle at Cerro Calan,National Astronomical Observatory, during the period 1989 to 1994, aregiven. The average mean square error of a position, for the wholeCatalogue, is +/-0.009 s. The mean epoch of the catalogue is 1991.84.
| Stroemgren photometry of F- and G-type stars brighter than V = 9.6. I. UVBY photometry
Within the framework of a large photometric observing program, designedto investigate the Galaxy's structure and evolution, Hβ photometryis being made for about 9000 stars. As a by-product, supplementary uvbyphotometry has been made. The results are presented in a cataloguecontaining 6924 uvby observations of 6190 stars, all south ofδ=+38deg. The overall internal rms errors of one observation(transformed to the standard system) of a program star in the interval6.5
|
הכנס מאמר חדש
לינקים קשורים
הכנס לינק חדש
משמש של הקבוצה הבאה
|
תצפית ומידע אסטרומטרי
| קבוצת-כוכבים: | יונה |
| התרוממות ימנית: | 05h11m29.52s |
| סירוב: | -33°52'50.4" |
| גודל גלוי: | 8.111 |
| מרחק: | 55.494 פארסק |
| תנועה נכונה: | -28.8 |
| תנועה נכונה: | -31 |
| B-T magnitude: | 8.956 |
| V-T magnitude: | 8.181 |
קטלוגים וכינוים:
|
