The Age of β Pictoris

Barrado, D.; Stauffer, J. R.; Song, Inseok; Caillault, J. P.

doi:10.1086/312162

Cited by 189 publications

(151 citation statements)

References 21 publications

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“…If we assume that the two components of the spectroscopic binary (HIP 96515 Aa & Ab) emit in X-rays, such that L x,Aa = L x,Ab = L x /2, and using the V-mag of each of the binary members (see Table 3) and the BC for a M1 and M2 star, we derive log(L x /L bol ) ratios of −3.17 and −3.04 for Aa and Ab, respectively. These values are comparable to those found in very active pre-main sequence (PMS) late-type stars (e.g., Barrado y Navascués et al 1999;Stelzer & Neuhäuser 2001) and in main-sequence (MS) late-type stars in very close binaries (see e.g. López-Morales 2007).…”

Section: Observational Properties Of Hip 96515 Aandbsupporting

confidence: 80%

The triple system HIP 96515: a low-mass eclipsing binary with a DB white dwarf companion

Huélamo¹,

Vaz

Torres

et al. 2009

A&A

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Context. HIP 96515 A is a double-lined spectroscopic binary included in the SACY catalog as a potential young star. It has a visual companion (CCDM 19371-5134 B, HIP 96515 B) at 8. 6. If bound to the primary, the optical and infrared colors of this wide companion are consistent with those of a white dwarf. Aims. We attempt to characterize the system HIP 96515 A&B by studying each of its components. Methods. We analyzed spectroscopic and photometric observations of HIP 96515 A and its visual companion, HIP 96515 B. To confirm the system as a common proper-motion pair, we analyzed the astrometry of the components using high-angular resolution infrared observations obtained within a time span of two years, and archival astrometry. Results. The high-resolution optical spectrum of HIP 96515 A was used to derive a mass ratio, M 2 /M 1 , close to 0.9. The optical lightcurve of HIP 96515 A shows periodic variations with P orbital = 2.3456 days, revealing that HIP 96515 A is an eclipsing binary with preliminary orbital parameters of i = 89.• 0 ± 0.• 2, and M 1 = 0.59 ± 0.03 M and M 2 = 0.54 ± 0.03 M , for the primary and secondary, respectively, at an estimated distance of 42 ± 3 pc. This is a new eclipsing binary with component masses below 0.6 M . Multi-epoch observations of HIP 96515 A&B show that the system is a common proper-motion pair. The optical spectrum of HIP 96515 B is consistent with a pure helium atmosphere (DB) white dwarf. The comparison with evolutionary cooling sequence models provides T eff,WD = 19 126 ± 195 K, log g WD = 8.08, M WD /M = 0.6, and a distance of ∼46 pc. The estimated WD cooling age is ∼100 Myr and the total age of the object (including the main-sequence phase) is ∼400 Myr. Finally, if HIP 96515 A&B are coeval, and assuming a common age of ∼400 Myr, the comparison of the masses of the eclipsing binary members with evolutionary tracks shows that they are underestimated by ∼15% and 10%, for the primary and secondary, respectively.

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Section: Observational Properties Of Hip 96515 Aandbsupporting

confidence: 80%

The triple system HIP 96515: a low-mass eclipsing binary with a DB white dwarf companion

Huélamo¹,

Vaz

Torres

et al. 2009

A&A

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“…Numerous investigations and reviews have targeted the three stars, which are among the youngest pre-main sequence stars in the solar neighbourhood. They display X-ray emission, flaring activity, flux excess in the infrared due to a circumstellar disc (AU Mic), photometric variability (of BY Dra type), active coronae, Ca ii H+K in emission, and other properties typical of young stars (Linsky et al 1982;Kundu et al 1987;Pallavicini et al 1990;Batalha et al 1996;Barrado y Navascués et al 1999;Katsova et al 1999;Zuckerman et al 2001;Kalas et al 2004). There is a difference between Hipparcos heliocentric distances of 0.8 ± 0.4 pc, which could be real (as in the case of α Cen AB and Proxima) or stem from a poor accuracy in the parallax measurement (e.g.…”

Section: Wds 20452-3120 (Au Mic and At Mic Ab)mentioning

confidence: 99%

Reaching the boundary between stellar kinematic groups and very wide binaries

Caballero¹

2009

A&A

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Aims. I look for and characterise very wide binaries and multiple systems with projected physical separations larger than s = 0.1 pc, which is generally believed to be a sharp upper limit to the distribution of wide binary semimajor axes. Methods. I investigated in detail 30 Washington double stars with angular separations of ρ > 1000 arcsec. I discarded 23 of them as probably unbound systems based on discordant astrometry, photometry, spectral types, and radial velocities. The remaining seven systems were subject to a comprehensive data compilation and derivation (multi-wavelength photometry, heliocentric distance, multiplicity, age, mass, metallicity, membership in a young kinematic group). Results. Of the seven very wide systems, six have projected physical separations greater than the hypothetical cutoff at s = 0.1 pc and four have separations s > 0.2 pc. Although there are two systems in young kinematic groups (namely HD 136654 and BD+32 2572 in the Hyades Supercluster, and AU Mic and AT Mic AB in the β Pictoris moving group), there is no clear prevalence of young systems (τ < 1 Ga) among these very wide binaries. Finally, I compare the binding energies of the seven systems with those of other weakly bound systems in the field.

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“…been determined from lower mass members of its comoving group (Barrado y Navascués et al 1999;Zuckerman et al 2001). Thus, b Pic is one of the youngest, closest stars to Earth.…”

Section: ϫ4mentioning

confidence: 99%

The First Spatially Resolved Mid-Infrared Spectroscopy of β Pictoris

Weinberger

Becklin

Zuckerman

2003

The Astrophysical Journal

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Long-slit spectra probe the southwest side of the disk in the 8-13 mm region. Dust within 0Љ .8 of the star shows silicate emission features, including amorphous and crystalline species. Farther out, the disk spectra are featureless and are entirely dominated by dust thermal continuum emission. Mid-infrared imaging of b Pictoris reveals spatial asymmetries in its dusty circumstellar disk at a spatial resolution of 0Љ .5. Visible for the first time is an inner ( AU) warp in the disk that is aligned differently from a larger scale warp observed in scattered light by r ! 20 the Hubble Space Telescope. At 12 mm, as has been observed before, the southwest extension of the disk is brighter than the northeast side. This asymmetry appears to be not as significant at 18 mm. The spatially resolved spectra show that this asymmetry cannot be accounted for by small dust grains that have a spectral feature.

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The Age of β Pictoris

Cited by 189 publications

References 21 publications

The triple system HIP 96515: a low-mass eclipsing binary with a DB white dwarf companion

The triple system HIP 96515: a low-mass eclipsing binary with a DB white dwarf companion

Reaching the boundary between stellar kinematic groups and very wide binaries

The First Spatially Resolved Mid-Infrared Spectroscopy of β Pictoris

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