Two families of exocomets in the β Pictoris system

  title={Two families of exocomets in the $\beta$ Pictoris system},
  author={Flavien Kiefer and Alain Lecavelier des Etangs and Jean-Louis Boissier and Alfred Vidal-Madjar and Herv'e Beust and Anne-Marie Lagrange and Guillaume H{\'e}brard and Roger Ferlet},
The young planetary system surrounding the star β Pictoris harbours active minor bodies. These asteroids and comets produce a large amount of dust and gas through collisions and evaporation, as happened early in the history of our Solar System. Spectroscopic observations of β Pictoris reveal a high rate of transits of small evaporating bodies, that is, exocomets. Here we report an analysis of more than 1,000 archival spectra gathered between 2003 and 2011, which provides a sample of about 6,000… 

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

  • G. Kennedy
  • Physics, Geology
    Monthly Notices of the Royal Astronomical Society
  • 2018
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

Exocomets from a Solar System Perspective

Exocomets are small bodies releasing gas and dust which orbit stars other than the Sun. Their existence was first inferred from the detection of variable absorption features in stellar spectra in the

Evidence for an additional planet in the β Pictoris system

With its imaged debris disk of dust, its evaporating exocomets, and an imaged giant planet, the young (~23 Myr) β Pictoris system is a unique proxy for detailed studies of planet formation processes

Exocomets size distribution in the [Formula: see text] Pictoris planetary system.

The star [Formula: see text] Pictoris harbors a young planetary system of about 20 million years old, which is characterized by the presence of a gaseous and dusty debris disk, at least two massive

E P ] 2 8 A pr 2 02 2 Exocomets size distribution in the β Pictoris planetary system

The star β Pictoris harbors a young planetary system, which is characterized by the presence of a gaseous and dusty debris disk1–6, at least two massive planets7–10 and many minor bodies. For more

Fe I in the β Pictoris circumstellar gas disk

The young planetary system β Pictoris is surrounded by a debris disk of dust and gas. The gas source of this disk could be exocomets (or “falling and evaporating bodies”, FEBs), which produce

Exocomets: A spectroscopic survey

Context. While exoplanets are now routinely detected, the detection of small bodies in extrasolar systems remains challenging. Since the discovery of sporadic events, which are interpreted to be

Exocomet Circumstellar Fe I Absorption in the Beta Pictoris Gas Disk

We present an archival study of 27 circumstellar Fe i (λ3860 Å) and Ca ii (λ3933 Å) absorption spectra of the β Pictoris system recorded over the 2003–2014 timeframe. We have detected several

Astronomy: Hurling comets around a planetary nursery

An analysis of hundreds of star-grazing comets in a young planetary system shows that they form two families: a group of old, dried-out comets and a younger group probably related to the break-up of

Transiting exocomets detected in broadband light by TESS in the β Pictoris system

Aims. We search for signs of falling evaporating bodies (FEBs, also known as exocomets) in photometric time series obtained for β Pictoris after fitting and removing its δ Scuti-type pulsation



An early extrasolar planetary system revealed by planetesimal belts in β Pictoris

It is reported that the sub-micrometre amorphous silicate grains around β Pic have peaks in their distribution around 6, 16 and 30’au (1 au is the Sun–Earth distance), whereas the crystalline and micrometr-sized amorphously silicategrain grains are concentrated in the disk centre.

Falling Evaporating Bodies as a Clue to Outline the Structure of the β Pictoris Young Planetary System

Transient redshifted events monitored in the spectrum offl Pictoris have been interpreted for many years as resulting from the evaporation of numerous comet-like bodies in the vicinity of this stars.

Deficiency of molecular hydrogen in the disk of β Pictoris

Molecular hydrogen (H2) is by far the most abundant material from which stars, protoplanetary disks and giant planets form, but it is difficult to detect directly. Infrared emission lines from H2

Stabilization of the disk around β Pictoris by extremely carbon-rich gas

The edge-on disk surrounding the nearby young star β Pictoris is the archetype of ‘debris disks’, which are composed of dust and gas produced by collisions between—and evaporation of—planetesimals,

Mean-Motion Resonances as a Source for Infalling Comets toward β Pictoris

Abstract Repeated time-variable redshifted absorption features in the spectrum of β Pictoris (β Pic) have been attributed to comet-like bodies falling toward the star, when evaporating in its

Falling evaporating bodies in the β Pictoris system - Resonance refilling and long term duration of the phenomenon

The transient spectral absorption events that have been monitored for years towards the star Pictoris have been interpreted as resulting from the transit across the line of sight of evaporating,

Comet-like mineralogy of olivine crystals in an extrasolar proto-Kuiper belt

The detection of the 69-micrometre-wavelength band of olivine crystals in the spectrum of β Pictoris shows values strikingly similar to those for the dust emitted by the most primitive comets in the Solar System, even though β’Pictoris is more massive and more luminous and has a different planetary system architecture.

Mid-infrared images of β Pictoris and the possible role of planetesimal collisions in the central disk

Thermal infrared images of the central disk imply that the brightness asymmetry results from the presence of a bright clump composed of particles that may differ in size from dust elsewhere in the disk, which is suggested to result from the collisional grinding of resonantly trapped planetesimals or the cataclysmic break-up of a planetesimal.

A hydrodynamical model for infalling evaporating bodies in the β Pictoris circumstellar disk

Abstract The temporal spectroscopic variations monitored since 1985 toward β Pictoris (β Pic) in both visible and UV lines have been formerly interpreted as the result of the vaporization, in the