Plasma Poynting-Roberson Effect on Fluffy Dust Aggregate

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Presentation transcript:

Plasma Poynting-Roberson Effect on Fluffy Dust Aggregate T. Yamamoto Inst. Low Temperature Sci., Hokkaido Univ. In collaboration with T. Minato, H. Kimura (ILTS, Hokkaido U.) I. Mann, M. Koelher (Inst. Planetologie, Muenster U.)

Dust around Young Main-Sequence Stars & in the Solar System Observed in debris disk around young MS stars (Vega-like stars) & in the present solar system Dust disk around βPic IDP captured in the Earth atmosphere

Dust around Young Main-Sequence Stars & in the Solar System Dust in debris disk around Vega-like stars Debris after formation of planetary systems? In situ production by collisions of planetesimals? Dust in the present solar system Supply from comets, asteroid collisions & inflow of interstellar dust Dust must be supplied because of the limitation of its life time

What limits the life time? Poynting-Roberson effect Photon PR effect Absorption and scattering of stellar photons Plasma PR effect Collisions of stellar wind ions

Forces acting on a dust particle gravity PR drag radiation/wind pressure star

PR drag Drag appears due to aberration on the particle in orbit Aberration angle

Ratio of the plasma and photon PR drags comparable to photon PR drag for the present solar system dominant for the young MS stars

Momentum transfer cross section For photons: Mie theory for spherical particles DDA, … for aggregates For charged particles: Spherical particles Mukai & Yamamoto 1982, A&A107, 97 Perfect absorption Minato et al. 2004, A&A, 424, L13 Stopping power is taken into account. Aggregates: Present study Any shape & structure Stopping power

Models of dust aggregates (Mukai et al. 1992, Kimura et al. 2002) BPCA　(Ballistic Particle-Cluster Aggregations) Fractal dimension BCCA (Ballistic Cluster-Cluster Aggregations) cf. IDP

Momentum transfer cross section Stopping power: Cross section : Distribution function of the thickness : Range of the incident stellar wind ions Small aggregates: Large aggregates: cf. radiation pressure cross section

Momentum transfer cross section averaged over the aggregate directions fluffyness geometrical cs penetration

Empirical formula aggregate spheroid Momentum transfer cs Approximated to be the cross section for a spheroid of the same V and S. aggregate spheroid

Dust around young main-sequence stars Life time: limited by the photon PR drag (previous study) Young MS stars High mass-loss rate: Luminosity: (Wood et al. 2002) Plasma PR drag will be dominant.

Life time against the PR drag spherical silicate 10 AU to the star photon Life time is shorter for the aggregates wind plasma

Implications Rate of dust supply should be much larger than the previous estimates Much larger number of planetesimals in the disk?

Mass loss rate vs the age of stars Wood et al. 2002

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