High latitude gas in the<i>β</i>Pictoris system

Beust, H.; Valiron, P.

doi:10.1051/0004-6361:20053425

Cited by 29 publications

(29 citation statements)

References 39 publications

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“…Beust & Valiron (2007) have shown that most FEBs would remain spectroscopically undetected if the β Pic disk was inclined by more that a few tens of degrees. This also applies to HD 172555 if the dynamical origin of the FEBs is the same.…”

Section: Discussionmentioning

confidence: 99%

Exocomets in the circumstellar gas disk of HD 172555

Kiefer

Étangs

Augereau

et al. 2014

A&A

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The source HD 172555 is a young A7V star surrounded by a debris disk with a gaseous component. Here, we present the detection of variable absorption features detected simultaneously in the Ca II K and H doublet lines (at λ3933 Å and λ3968 Å). We identified the presence of these absorption signatures at four different epochs in the 129 HARPS high-resolution spectra gathered between 2004 and 2011. These transient absorption features are most likely due to falling evaporating bodies (FEBs, or exocomets) that produce absorbing gas observed transiting in front of the central star. We also detect a stable Ca II absorption component at the star's radial velocity. With no corresponding detection in the Na I line, the resulting very low upper limit for the Na I/Ca II ratio suggests that this absorption is due to circumstellar gas.

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Section: Discussionmentioning

confidence: 99%

Exocomets in the circumstellar gas disk of HD 172555

Kiefer

Étangs

Augereau

et al. 2014

A&A

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“…Their origin has been tentatively related to mean-motion resonances with a Jovian planet orbiting the star (Beust & Morbidelli 1996Thébault & Beust 2001;Beust & Valiron 2007). Several constraints have been deduced from dynamical studies of the FEBs scenario, suggesting that:…”

Section: The β Pic Cometary Activitymentioning

confidence: 99%

Orbital characterization of theβPictoris b giant planet

Chauvin¹,

Lagrange²,

Beust³

et al. 2012

A&A

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156

221

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Context. In June 2010, we confirmed the existence of a giant planet in the disk of the young star β Pictoris located between 8 AU and 15 AU from the star. This young planet offers the rare opportunity to monitor a large fraction of the orbit using the imaging technique over a reasonably short timescale. It also offers the opportunity to study its atmospheric properties using spectroscopy and multi-band photometry, and possibly derive its dynamical mass by combining imaging with radial velocity data to set tight constraints on giant planet formation theories. Aims. We aim to measure the evolution of the planet's position relative to the star β Pictoris to determine the planetary orbital properties. Our ultimate goal is to relate both the planetary orbital configuration and physical properties to either the disk structure or the cometary activity observed for decades in the β Pictoris system. Methods. Using the NAOS-CONICA adaptive-optics instrument (NACO) at the Very Large Telescope (VLT), we obtained repeated follow-up images of the β Pictoris system in the K s and L filters at four new epochs in 2010 and 2011. Complementing these data with previous measurements, we conduct a homogeneous analysis, which covers more than eight yrs, to accurately monitor the β Pictoris b position relative to the star. We then carefully consider the various sources of uncertainties that may affect the orbital parameter determination. Results. On the basis of the evolution of the planet's relative position with time, we derive the best-fit orbital solutions for our measurements using two fitting methods, a least squares Levenberg-Marquardt algorithm and a Markov-chain Monte Carlo approach. More reliable results are found with the second approach as our measurements do not cover the complete planetary orbit, and are biased toward the most recent epochs since the planet recovery. The solutions favor a low-eccentricity orbit e < ∼ 0.17, with semi-major axis in the range 8-9 AU corresponding to orbital periods of 17-21 yrs. Our solutions favor a highly inclined solution with a peak around i = 88.5 ± 1.7 • , and a longitude of ascending node tightly constrained at Ω = −147.5 ± 1.5 • . These results indicate that the orbital plane of the planet is likely to be above the midplane of the main disk, and compatible with the warp component of the disk being tilted between 3.5 deg and 4.0 deg. This suggests that the planet plays a key role in the origin of the inner warped-disk morphology of the β Pic disk. Finally, these orbital parameters are consistent with the hypothesis that the planet is responsible for the transit-like event observed in November 1981, and also linked to the cometary activity observed in the β Pic system.

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“…The star hosts an ∼1000-AU-wide gas-rich debris disk (Smith & Terrile 1984) presented nearly edge-on. Asymmetries in the disk and variability in high-resolution spectra indicative of dynamic comets (Kiefer et al 2014) suggested the presence of one or more planets long before the discovery of β Pic b itself (Lagrange-Henri et al 1988;Beust et al 1990;Roques et al 1993;Levison et al 1994;Mouillet et al 1997;Freistetter et al 2007;Beust & Valiron 2007). Finally, the giant exoplanet β Pic b was imaged (Lagrange et al 2009) and confirmed (Lagrange et al 2010) using adaptive optics (AO) at VLT/NaCo.…”

Section: Introductionmentioning

confidence: 97%

MAGELLAN ADAPTIVE OPTICS FIRST-LIGHT OBSERVATIONS OF THE EXOPLANETβPIC b. II. 3–5μm DIRECT IMAGING WITH MagAO+Clio, AND THE EMPIRICAL BOLOMETRIC LUMINOSITY OF A SELF-LUMINOUS GIANT PLANET

Morzinski

Males

Skemer

et al. 2015

ApJ

124

123

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Young giant exoplanets are a unique laboratory for understanding cool, low-gravity atmospheres. A quintessential example is the massive extrasolar planet β Pic b, which is 9 AU from and embedded in the debris disk of the young nearby A6V star β Pictoris. We observed the system with first light of the Magellan Adaptive Optics (MagAO) system. In Paper I (Males et al. 2014) we presented the first CCD detection of this planet with MagAO+VisAO. Here we present four MagAO+Clio images of β Pic b at 3.1 µm, 3.3 µm, L ′ , and M ′ , including the first observation in the fundamental CH 4 band. To remove systematic errors from the spectral energy distribution (SED), we re-calibrate the literature photometry and combine it with our own data, for a total of 22 independent measurements at 16 passbands from 0.99-4.8 µm. Atmosphere models demonstrate the planet is cloudy but are degenerate in effective temperature and radius. The measured SED now covers >80% of the planet's energy, so we approach the bolometric luminosity empirically. We calculate the luminosity by extending the measured SED with a blackbody and integrating to find log(L bol /L ⊙ ) = −3.78 ± 0.03. From our bolometric luminosity and an age of 23±3 Myr, hot-start evolutionary tracks give a mass of 12.7±0.3 M Jup , radius of 1.45±0.02 R Jup , and T eff of 1708±23 K (model-dependent errors not included). Our empirically-determined luminosity is in agreement with values from atmospheric models (typically −3.8 dex), but brighter than values from the field-dwarf bolometric correction (typically −3.9 dex), illustrating the limitations in comparing young exoplanets to old brown dwarfs.

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High latitude gas in theβPictoris system

Cited by 29 publications

References 39 publications

Exocomets in the circumstellar gas disk of HD 172555

Exocomets in the circumstellar gas disk of HD 172555

Orbital characterization of theβPictoris b giant planet

MAGELLAN ADAPTIVE OPTICS FIRST-LIGHT OBSERVATIONS OF THE EXOPLANETβPIC b. II. 3–5μm DIRECT IMAGING WITH MagAO+Clio, AND THE EMPIRICAL BOLOMETRIC LUMINOSITY OF A SELF-LUMINOUS GIANT PLANET

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