Detecting the Dusty Debris of Terrestrial Planet Formation

2004/01/16 by Scott J. Kenyon, Scott J Kenyon, Benjamin C. Bromley +1 · 5 citations
Physics and Astronomy · #Accretion (finance) #Astro and Planetary Science #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Debris #Debris disk #Planet #Solar System #Terrestrial planet #astro-ph

paper · pdf · doi:10.1086/382693

published as Astrophys.J. 602 (2004) L133-L136 · 11 pages of text, 3 figures, accepted for ApJ Letters, additional info at http://cfa-www.harvard.edu/~kenyon/pf/terra/td1

arxiv created 2004/01/16 · openalex publication_date 2004/02/05 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

We use a multiannulus accretion code to investigate debris disks in the terrestrial zone at 0.7-1.3 AU around a 1 M ☉ star. Terrestrial planet formation produces a bright dusty ring of debris with a lifetime of ≳10 6 yr. The early phases of terrestrial planet formation are observable with current facilities; the late stages require more advanced instruments with adaptive optics.

Citations

• The Formation of Planetesimals
• The distribution of mass in the planetary system and solar nebula
• Accretion Disks around Young Objects. III. Grain Growth
• Accretion in the Early Kuiper Belt. II. Fragmentation
• Disk Frequencies and Lifetimes in Young Clusters
• Dusty Debris Around Solar-Type Stars: Temporal Disk Evolution
• ISOCAM observations of the ρ Ophiuchi cloud: Luminosity and mass functions of the pre-main sequence embedded cluster
• Planet Formation

Cited by

• A Search for Warm Circumstellar Disks in the TW Hydrae Association
• New M Dwarf Debris Disk Candidates in NGC 2547
• The Formation and Evolution of Planetary Systems (FEPS): Discovery of an Unusual Debris System Associated with HD 12039
• FORMATION OF SUPER-EARTH MASS PLANETS AT 125–250 AU FROM A SOLAR-TYPE STAR
• FORMATION AND EVOLUTION OF PLANETARY SYSTEMS: PROPERTIES OF DEBRIS DUST AROUND SOLAR-TYPE STARS
• Terrestrial Planet Formation. I. The Transition from Oligarchic Growth to Chaotic Growth