F, G and K stars in the ROSAT all-sky 
survey

Metanomski, A.; Pasquini, L.; Krautter, J.; Cutispoto, G.; Fleming, T. A.

doi:10.1051/aas:1998431

Cited by 10 publications

(15 citation statements)

References 14 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These new data have been now taken into account computing the spectral type listed in Table 4. In most cases the spectral types obtained from color indices agree very well with the spectral classification, when available, as also shown for a larger sample of late-type stars by Metanomski et al (1997).…”

Section: Resultssupporting

confidence: 75%

Long-term monitoring of active stars

Cutispoto

1998

Astron. Astrophys. Suppl. Ser.

Self Cite

View full text Add to dashboard Cite

Abstract. In the framework of an extensive program focusing on the global properties and evolution of active stars, high-precision UBV (RI) c photometry of 19 selected stars, collected at the European Southern Observatory over the 15-31 March 1991 interval is presented. Significant evolution of the light curves, period variations and evidence for long-term variability of the global degree of spottedness are found. Most of the spectral classifications are discussed. A flare event was detected for the star HD 127535 = V 841 Cen. These observations contribute to the establishment of a time-extended photometric database which can give important clues on topics such as the stability of spotted areas, differential rotation, solar-like cycles and the correlation between inhomogeneities at different atmospheric levels 1 .

show abstract

Section: Resultssupporting

confidence: 75%

Long-term monitoring of active stars

Cutispoto

1998

Astron. Astrophys. Suppl. Ser.

Self Cite

View full text Add to dashboard Cite

show abstract

“…The lack of candidate systems within the Gliese catalogue stars then, at least somewhat, validates the pre-LMXB selection criteria, as you would not expect to find any such systems within the local space volume. Furthermore, the best four candidate pre-LMXB systems, to date, are at distances of 205 þ30 220 pc, 445 þ78 254 pc, 449 þ78 252 pc and 506 þ116 2075 pc [for the first four objects in Table 6 respectively (Metanomski et al 1998)], consistent with that expected for such systems. If the LMXB and pre-LMXB number populations are similar, then we would expect pre-LMXB systems to be located at comparable distances to LMXBs with neutron star accretors.…”

Section: D E N T I F I C At I O N a N D Discussion O F C Asupporting

confidence: 70%

“… * Absolute visual magnitudes ( M V ) were calculated using the apparent visual magnitudes ( V ) and distances from Metanomski et al (1998). The values of absolute visual magnitude and X‐ray luminosity ( L X ) can be employed with reference to, for example, fig.…”

Section: Identification and Discussion Of Candidate Pre‐lmxb Systemsmentioning

confidence: 99%

A possible detection mechanism for pre-low-mass X-ray binaries

Bleach

2002

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

This work presents a possible detection mechanism for close, detached, neutron star–red dwarf binaries, which are expected to be the evolutionary precursors of low‐mass X‐ray binaries (LMXBs). Although this pre‐low‐mass X‐ray binary (pre‐LMXB) phase of evolution is predicted theoretically, as yet no such systems have been identified observationally. The calculations presented here suggest that the X‐ray luminosity of neutron star wind accretion in a pre‐LMXB system can be expected to exceed the intrinsic X‐ray luminosity of the red dwarf secondary star. Furthermore, the temperature of the radiation emitted from the neutron star wind accretion process is expected, within the confines of a reasonable set of conditions, to lie within the detection range of X‐ray satellites. Sources with X‐ray luminosities greater than that expected for a red dwarf star, but the positions of which coincide with that of a red dwarf star, are then candidate pre‐LMXB systems. These candidate systems should be surveyed for the radial velocity shifts that would occur as a result of the orbital motion of a red dwarf star within a close binary system containing a high‐mass compact object.

show abstract

“…Errors are of the order of 0.01 magnitudes. The symbol ":" denotes errors of the order of 0.02 magnitudes; the epochs of observation are given in Table 1 c or ck shown by Metanomski et al (1998), the last version can be successfully applied also for specific objects (see par. 3 in Cutispoto 1998b).…”

Section: Resultsmentioning

confidence: 99%

Long-term monitoring of active stars

Cutispoto¹,

Messina²,

Rodonò³

2001

A&A

Self Cite

View full text Add to dashboard Cite

Abstract. As a part of an extensive program focused on the global properties and evolution of active stars, high-precision UBV (RI)c and UBV photometry of 31 selected stars is presented. The UBV (RI)c observations were collected at the European Southern Observatory over the 31 December 1992-18 January 1993 and the 20 November-3 December 1993 intervals. Additional UBV photometry obtained by the "Phoenix" and by the Catania Astrophysical Observatory Automatic Photoelectric Telescopes from 1990 to 1993 is also presented for some of the program stars. Significant evolution of the light curves, period variations and evidence for longterm variability of the global degree of spottedness are found. Some spectral classifications are revised and the inferred photometric parallaxes are compared, whenever possible, with the values measured by the Hipparcos satellite. These observations are finalized to the construction of an extended photometric database, which can give important clues on topics such as the stability of spotted areas, differential rotation, solar-like cycles and the correlation between inhomogeneities at different atmospheric levels.

show abstract

F, G and K stars in the ROSAT all-sky survey

Cited by 10 publications

References 14 publications

Long-term monitoring of active stars

Long-term monitoring of active stars

A possible detection mechanism for pre-low-mass X-ray binaries

Long-term monitoring of active stars

Contact Info

Product

Resources

About