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Classification of Spectra from the Infrared Space Observatory PHT-S Database
We have classified over 1500 infrared spectra obtained with the PHT-Sspectrometer aboard the Infrared Space Observatory according to thesystem developed for the Short Wavelength Spectrometer (SWS) spectra byKraemer et al. The majority of these spectra contribute to subclassesthat are either underrepresented in the SWS spectral database or containsources that are too faint, such as M dwarfs, to have been observed byeither the SWS or the Infrared Astronomical Satellite Low ResolutionSpectrometer. There is strong overall agreement about the chemistry ofobjects observed with both instruments. Discrepancies can usually betraced to the different wavelength ranges and sensitivities of theinstruments. Finally, a large subset of the observations (~=250 spectra)exhibit a featureless, red continuum that is consistent with emissionfrom zodiacal dust and suggest directions for further analysis of thisserendipitous measurement of the zodiacal background.Based on observations with the Infrared Space Observatory (ISO), aEuropean Space Agency (ESA) project with instruments funded by ESAMember States (especially the Principle Investigator countries: France,Germany, Netherlands, and United Kingdom) and with the participation ofthe Institute of Space and Astronautical Science (ISAS) and the NationalAeronautics and Space Administration (NASA).
| Chromospherically Active Stars. XXII. HD 18955, A Massive K Dwarf Binary
HD 18955 is a double-lined spectroscopic binary with a period of 43.3214days and a high eccentricity of 0.761. The spectral types of thecomponents are K0 V and K2-K3 V. The secondary is a typical early Kdwarf, although its minimum mass is greater than canonical values.However, this larger mass is consistent with other early K dwarf,spectroscopic binary results. The primary is anomalous, beingsubstantially underluminous for its radius and mass, which are equal toor slightly greater than solar values. A lack of lithium argues that thecomponents are not pre-main-sequence stars. The large minimum masses ofboth components suggest that the system has a high orbital inclination.Our photometric observations around the times of conjunction show noevidence of eclipses, but considering the uncertainties in theephemerides, there is only a 50% chance that our photometricobservations would have detected the primary eclipse and almost nochance that we covered the secondary eclipse. Hence, eclipses remain areal possibility in this system. Photometric variations with anamplitude of 0.02 mag reveal a period of 7.55 days, which is assumed tobe the primary star's rotation period. Thus, given the spectral types ofthe stars, this system is a BY Draconis type variable. With vsini valuesof 5 km s-1 for both components, the two stars are rotatingmore rapidly than typical K dwarf field stars, but the observed rotationperiod is still substantially longer than the predictedpseudosynchronous rotation period of 4.6 days for the primary.
| Long-term monitoring of active stars. IX. Photometry collected in 1993
As a part of an extensive program focused on the global properties andevolution of active stars, high-precision UBV(RI)_c and UBV photometryof 31 selected stars is presented. The UBV(RI)_c observations werecollected at the European Southern Observatory over the 31 December1992-18 January 1993 and the 20 November-3 December 1993 intervals.Additional UBV photometry obtained by the ``Phoenix" and by the CataniaAstrophysical Observatory Automatic Photoelectric Telescopes from 1990to 1993 is also presented for some of the program stars. Significantevolution of the light curves, period variations and evidence forlong-term variability of the global degree of spottedness are found.Some spectral classifications are revised and the inferred photometricparallaxes are compared, whenever possible, with the values measured bythe Hipparcos satellite. These observations are finalized to theconstruction of an extended photometric database, which can giveimportant clues on topics such as the stability of spotted areas,differential rotation, solar-like cycles and the correlation betweeninhomogeneities at different atmospheric levels. Based on data collectedat the European Southern Observatory, La Silla, Chile. Tables and thecomplete data set are also available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/367/910
| Long-term monitoring of active stars. IV. UBV(RI)_c_ observations obtained at La Silla in December 1989.
High-precision UBV(RI)_c_ photometry of 23 selected acitve stars,collected at the European Southern Observatory (La Silla, Chile) overthe period 9-28 December 1989, is presented. This paper is part of alarger program focusing on the global properties and evolution of activestars and is aimed at establishing a time-extended database which cangive important clues on topics such as the stability of the spottedareas, differential rotation and solar-like cycles. Significantevolution of the wave-like light curves, period variations and, in mostcases, evidence for long-term variability of the global degree ofspottedness are found for the observed stars. Some spectralclassifications are rediscussed and evidence for a newly discoveredvariable star is given.
| Long-term monitoring of active stars. II - UBV(RI)c observations at ESO during January-March 1989
In the framework of a research program focusing on the global propertiesand evolution of photospheres and outer atmospheres of active stars, theauthor presents high-precision UBV(RI)c photometry of 15 selected RSCVn, BY Dra, and FK Com-type systems observed at the European SouthernObservatory (La Silla, Chile) in the period January-March 1989.Significant evolution both in amplitude and shape of the wave-like lightcurves is found with respect to previous observations. Evidence forlong-term variability for most of the observed stars is also presented,and some of the spectral classifications are rediscussed.
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| Takýmyýldýz: | Irmak |
| Sað Açýklýk: | 02h58m12.55s |
| Yükselim: | -12°00'21.0" |
| Görünürdeki Parlaklýk: | 6.509 |
| Uzaklýk: | 128.205 parsek |
| özdevim Sað Açýklýk: | 10.3 |
| özdevim Yükselim: | -11.6 |
| B-T magnitude: | 7.823 |
| V-T magnitude: | 6.618 |
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