Classification of EUV stellar sources detected by the ROSAT 
WFC

Cutispoto, G.; Pastori, L.; Tagliaferri, G.; Messina, S.; Pallavicini, R.

doi:10.1051/aas:1999497

Cited by 47 publications

(94 citation statements)

References 37 publications

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“…This would indicate a quadruple system. However, we note that the v sin i values of the two components in Cutispoto et al (1999) are roughly exchanged with respect to other studies in the literature (Table A.1). An analysis of the CES spectra used in Cutispoto et al (1999) indicates that the components were indeed exchanged in the original study.…”

Section: Appendix B: Notes On Individual Objectsmentioning

confidence: 43%

“…We also analyzed the CES spectra of the components of HD 16699 A and B obtained by Cutispoto et al (1999; kindly provided by L. Pastori) to understand the origin of discrepancies between results from the literature and results from our own analysis, which turned out to be due to an exchange of binary system components (see Appendix B for details).…”

Section: Other Datamentioning

confidence: 99%

“…There is an additional component (HIP 12326 = HD 16699) at 8.7 arcsec, corresponding to a projected separation of 530 AU. According to Cutispoto et al (1999), HD 16699 shows a composite spectrum, with one system of sharp lines and another system of broad lines superimposed. Since the RV is constant, this was interpreted as being due to a companion at moderately large separation.…”

Section: Appendix B: Notes On Individual Objectsmentioning

confidence: 99%

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The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits

Desidera

Covino

Messina

et al. 2015

A&A

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Context. Young, close stars are ideal targets for searching planets using the direct imaging technique. The determination of stellar parameters is crucial for the interpretation of imaging survey results, particularly since the luminosity of substellar objects has a strong dependence on system age. Aims. We have conducted a large program with NaCo at the VLT to search for planets and brown dwarfs in wide orbits around 86 stars. A large fraction of the targets observed with NaCo were poorly investigated in the literature. We performed a study to characterize the fundamental properties (age, distance, and mass) of the stars in our sample. To improve target age determinations, we compiled and analyzed a complete set of age diagnostics. Methods. We measured spectroscopic parameters and age diagnostics using dedicated observations acquired with FEROS and CORALIE spectrographs at La Silla Observatory. We also made extensive use of archival spectroscopic data and the results that are available in the literature. Additionally, we exploited photometric time-series, which are available in ASAS and Super-WASP archives, to derive a rotational period for a large fraction of our program stars. Results. We provided updated characterization of all the targets observed in the VLT NaCo Large program, a survey designed to probe the occurrence of exoplanets and brown dwarfs in wide orbits. The median distance and age of our program stars are 64 pc and 100 Myr, respectively. Nearly all the stars have masses between 0.70 and 1.50 M , with a median value of 1.01 M . The typical metallicity is close to solar with a dispersion that is smaller than that of samples usually observed in radial velocity surveys. Several stars are confirmed or proposed here to be members of close young moving groups. Eight spectroscopic binaries are identified.

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Section: Appendix B: Notes On Individual Objectsmentioning

confidence: 43%

Section: Other Datamentioning

confidence: 99%

Section: Appendix B: Notes On Individual Objectsmentioning

confidence: 99%

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The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits

Desidera

Covino

Messina

et al. 2015

A&A

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“…The star is slowly rotating (V sin i < 5 km s −1 ; Cutispoto et al 1999). Should the 30 d photometric variability be due to rotation, a value of ∼1 km s −1 for the rotational velocity would result from the radius of 3.8 R derived in (Siess et al 2014) for IP Eri.…”

Section: The Ip Eri Systemmentioning

confidence: 99%

IP Eridani: A surprising long-period binary system hosting a He white dwarf

Merle

Jorissen

Masseron

et al. 2014

A&A

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We determine the orbital elements for the K0 IV + white dwarf (WD) system IP Eri, which appears to have a surprisingly long period of 1071 d and a significant eccentricity of 0.25. Previous spectroscopic analyses of the WD, based on a distance of 101 pc inferred from its Hipparcos parallax, yielded a mass of only 0.43 M , implying it to be a helium-core WD. The orbital properties of IP Eri are similar to those of the newly discovered long-period subdwarf B star (sdB) binaries, which involve stars with Heburning cores surrounded by extremely thin H envelopes, and are therefore close relatives to He WDs. We performed a spectroscopic analysis of high-resolution spectra from the HERMES/Mercator spectrograph and concluded that the atmospheric parameters of the K0 component are T eff = 4960 K, log g = 3.3, [Fe/H] = 0.09 and ξ = 1.5 km s −1 . The detailed abundance analysis focuses on C, N, O abundances, carbon isotopic ratio, light (Na, Mg, Al, Si, Ca, Ti) and s-process (Sr, Y, Zr, Ba, La, Ce, Nd) elements. We conclude that IP Eri abundances agree with those of normal field stars of the same metallicity. The long period and non-null eccentricity indicate that this system cannot be the end product of a common-envelope phase; it calls instead for another less catastrophic binary-evolution channel presented in detail in a companion paper.

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“…Over the past several decades, satellite surveys at X-ray and ultraviolet wavelengths have provided another very effective way of finding active, late-type stars. The observations produced by satellites such as HEAO-1, Einstein, EXOSAT, the Extreme Ultraviolet Explorer (EUVE ), and ROSAT have led to optical identifications (e.g., Buckley et al 1987;Fleming et al 1989;Cutispoto et al 1991Cutispoto et al , 1999Tagliaferri et al 1994;Jeffries et al 1995;Neuhaüser et al 1997) of many chromospherically active stars. Here we discuss three stars discovered from objective-prism spectra (Bidelman & MacConnell 1973;Bidelman 1981).…”

Section: Introductionmentioning

confidence: 99%

Chromospherically Active Stars. XXIV. The Giant, Single-lined Binaries HD 37824, HD 181809, and HD 217188

Fekel

Henry

2005

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We have obtained spectroscopy and photometry of three chromospherically active, single-lined spectroscopic binaries, HD 37824 (V1149 Ori), HD 181809 (V4138 Sgr), and HD 217188 (AZ Psc). HD 37824 has a circular orbit with a period of 53.57 days. Its primary is a K0 III star, while the secondary is likely a G or K dwarf. HD 181809 has an orbit with a period of 13.04667 days and a low eccentricity of 0.040. The primary has a spectral type of K0 III-IV, and its secondary is probably an M dwarf. The orbit of HD 217188 has a period of 47.1209 days and a moderately high eccentricity of 0.470. The spectral type of the primary is K0 III, while the secondary is likely an M dwarf. All three systems are estimated to have near solar iron abundances. Photometric observations spanning 15-16 years for all three stars yield mean photometric periods of 53.12, 59.85, and 90.89 days for HD 37824, HD 181809, and HD 217188, respectively. Thus, HD 37824 is rotating synchronously with the orbital period, while HD 181809 and HD 217188 are both rotating considerably slower than synchronously. All three stars show longterm variations in mean brightness and photometric amplitude, but no correlations are observed between the seasonal mean brightness, photometric amplitude, and seasonal photometric period in any of the stars. No clear evidence for long-term periodic variations in any of these parameters is present. The circular orbit of HD 37824 and the synchronous rotation of its K giant argue that the star is in the core helium-burning phase of its evolution. The giant components of HD 181809 and HD 217188 are asynchronous rotators, and both systems have eccentric orbits. Thus, those two stars are likely first-ascent giants.

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Classification of EUV stellar sources detected by the ROSAT WFC

Cited by 47 publications

References 37 publications

The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits

The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits

IP Eridani: A surprising long-period binary system hosting a He white dwarf

Chromospherically Active Stars. XXIV. The Giant, Single-lined Binaries HD 37824, HD 181809, and HD 217188

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