DUST AND POLYCYCLIC AROMATIC HYDROCARBON IN THE HD 34700 DEBRIS DISK

ABSTRACT The debris disk around the Vega-type star HD 34700 is detected in dust thermal emission from the near-infrared (IR) to millimeter (mm) and submm wavelength range. Also detected is a distinct set of emission features at 3.3, 6.2, 7.7, 8.6, 11.3, and , which are commonly attributed to polycyc...

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Bibliographic Details
Published in:The Astrophysical journal 2015-08, Vol.809 (1), p.1-10
Main Authors: Seok, Ji Yeon, Li, Aigen
Format: Article
Language:English
Subjects:
Accretion disks
ASTEROIDS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
circumstellar matter
COSMIC DUST
Debris
Disks
DISSOCIATION
Drag
Dust
ELEMENT ABUNDANCE
EMISSION
ENERGY SPECTRA
INFRARED RADIATION
infrared: stars
MOLECULES
PHOTOLYSIS
Polyallylamine hydrochloride
POLYCYCLIC AROMATIC HYDROCARBONS
POROUS MATERIALS
STARS
stars: individual (HD 34700)
STELLAR RADIATION
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Summary:ABSTRACT The debris disk around the Vega-type star HD 34700 is detected in dust thermal emission from the near-infrared (IR) to millimeter (mm) and submm wavelength range. Also detected is a distinct set of emission features at 3.3, 6.2, 7.7, 8.6, 11.3, and , which are commonly attributed to polycyclic aromatic hydrocarbon (PAH) molecules. We model the observed dust IR spectral energy distribution (SED) and PAH emission features of the HD 34700 disk in terms of porous dust and astronomical-PAHs. Porous dust together with a mixture of neutral and ionized PAHs closely explains the dust IR SED and PAH emission features observed in the HD 34700 disk. Due to the stellar radiation pressure and Poynting-Robertson drag together with the photodissociation of PAHs, substantial removal of dust and PAHs has occurred in the disk, and continuous replenishment of these materials is required to maintain their current abundances. This implies that these materials are not primitive but secondary products probably originating from mutual collisions among planetesimals, asteroids, and comets.
ISSN:0004-637X
1538-4357
1538-4357
DOI:10.1088/0004-637X/809/1/22