Pictoris: the variable Ca II H &amp; K absorptions from 1994 to 1996

Petterson, O. K. L.; Tobin, William

doi:10.1046/j.1365-8711.1999.02262.x

Cited by 18 publications

(32 citation statements)

References 18 publications

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“…Freistetter et al 2007). The main indirect indicators are (i) the inner warped component of the β Pic circumstellar disk, together with additional asymmetries observed in the outer part (Mouillet et al 1997;Kalas & Jewitt 1995); (ii) the photometric transit-like event observed in 1981 (Lecavelier des Etangs et al 1997); and (iii) the cometary activity observed in the absorption spectrum of β Pic (Ferlet et al 1987;Lagrange et al 1996;VidalMadjar et al 1998;Petterson & Tobin 1999). We discuss below how each of these observational findings may be related to both the existence and the orbital and physical properties of β Pic b.…”

Section: Discussionmentioning

confidence: 99%

“…Transient redshifted spectral events have been regularly monitored in the absorption spectrum of β Pic (Ferlet et al 1987;Lagrange et al 1996;Vidal-Madjar et al 1998;Petterson & Tobin 1999), and attributed to the sublimation of numerous stargrazing planetesimals crossing the line of sight, which are referred to the falling evaporating bodies (FEBs) phenomenon. 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).…”

Section: The β Pic Cometary Activitymentioning

confidence: 99%

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Orbital characterization of theβPictoris b giant planet

Chauvin¹,

Lagrange²,

Beust³

et al. 2012

A&A

153

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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Section: Discussionmentioning

confidence: 99%

Section: The β Pic Cometary Activitymentioning

confidence: 99%

Orbital characterization of theβPictoris b giant planet

Chauvin¹,

Lagrange²,

Beust³

et al. 2012

A&A

153

221

View full text Add to dashboard Cite

show abstract

“…In addition to these radio observations, optical surveys have revealed gas in the the debris disk systems HR 10 (Lagrange- Henri et al 1990), HD 32297 (Redfield 2007), 49 Ceti and ι Cyg (Montgomery & Welsh 2012), HD 2160, HD 110411, HD 145964, HD 183324 (Welsh & Montgomery 2013), and HD 17255 (Kiefer et al 2014). β Pic has been extensively studied using FUV/ optical gas tracers (e.g., Petterson & Tobin 1999;Roberge et al 2000Roberge et al , 2006Brandeker et al 2004) revealing a variable gas component due to the evaporation of comet-like bodies as they approach the central star. Far-infrared gas emission lines have also been detected by Herschel around HD172555 (Riviere-Marichalar et al 2012) and HD 32297 (Donaldson et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Flaherty

Hughes

Andrews

et al. 2016

ApJ

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The disk around HD 141569 is one of a handful of systems whose weak infrared emission is consistent with a debris disk, but still has a significant reservoir of gas. Here we report spatially resolved millimeter observations of the CO(3-2) and CO(1-0) emission as seen with the Submillimeter Array and CARMA. We find that the excitation temperature for CO is lower than expected from cospatial blackbody grains, similar to previous observations of analogous systems, and derive a gas mass that lies between that of gas-rich primordial disks and gas-poor debris disks. The data also indicate a large inner hole in the CO gas distribution and an outer radius that lies interior to the outer scattered light rings. This spatial distribution, with the dust rings just outside the gaseous disk, is consistent with the expected interactions between gas and dust in an optically thin disk. This indicates that gas can have a significant effect on the location of the dust within debris disks.

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“…Aside from the expectation of acceleration given the likely orbits, hints that it should be detectable can be seen in previous works; Ferlet et al (1987) show a series of spectra taken over several hours, in which a redshifted line clearly accelerates by about 5 km s −1 , and temporal variation was also seen by Lagrange et al (1996) and Petterson & Tobin (1999) With the detection of such an acceleration, the distance derived from is thought to originate in a stable circumstellar disc, while the varying components are attributed to exocomet comae. Features at both low and high velocity are seen, with those at low velocity tending to be deeper.…”

Section: Motivationmentioning

confidence: 55%

“…the optical depth can be estimated from the line ratios, e.g. Lagrange-Henri et al 1992;Petterson & Tobin 1999).…”

Section: Detection Of Exocomet Accelerationmentioning

confidence: 99%

Exocomet orbit fitting: accelerating coma absorption during transits of β Pictoris

Kennedy

2018

Monthly Notices of the Royal Astronomical Society

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Comets are a remarkable feature in our night sky, visible on their passage through the inner Solar system as the Sun's energy sublimates ices and liberates surface material, generating beautiful comae, dust, and ion tails. Comets are also thought to orbit other stars, and are the most promising interpretation of sporadic absorption features (i.e. transits) seen in spectra of stars such as β Pictoris and 49 Ceti. These "exocomets" are thought to form and evolve in the same way as in the Solar system, and as in the Solar system we may gain insight into their origins by deriving their orbits. In the case of β Pictoris, orbits have been estimated indirectly, using the radial velocity of the absorption features coupled with a physical evaporation model to estimate the stellocentric distance at transit d tr . Here, we note that the inferred d tr imply that some absorption signatures should accelerate over several hours, and show that this acceleration is indeed seen in HARPS spectra. This new constraint means that orbital characteristics can be obtained directly, and the pericentre distance and longitude constrained when parabolic orbits are assumed. The results from fitting orbits to 12 accelerating features, and a handful of non-accelerating ones, are in broad agreement with previous estimates based on an evaporation model, thereby providing some validation of the exocomet hypothesis. A prediction of the evaporation model, that coma absorption is deeper for more distant transits, is also seen here.

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Pictoris: the variable Ca II H & K absorptions from 1994 to 1996

Cited by 18 publications

References 18 publications

Orbital characterization of theβPictoris b giant planet

Orbital characterization of theβPictoris b giant planet

Resolved Co Gas Interior to the Dust Rings of the Hd 141569 Disk

Exocomet orbit fitting: accelerating coma absorption during transits of β Pictoris

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