flared disk gerde-ye borun-gošâ, disk-e ~ Fr.: disque évasé A model of → accretion disk around a
→ pre-main sequence star or
a → protostar in which the ratio of the
disk thickness to the distance from the star increases outward.
Current models of the irradiation of flared disks by stellar radiation predict that
a central hole is created around the young star due to the evaporation of
dust by the stellar radiation. The inner rim of the disk, at 0.5 to 1 AU from
the star, is irradiated by the star “frontally” (at 90° angle).
The heat produced by the irradiation causes
the inner rim to puff up. A part of the disk, from about 1 to 6 AU, lies in
the shadow of the puffed-up inner rim. The surface layers in this region do not
receive stellar photons directly. Therefore, there is no significant heating of the disk
midplane by reprocessed stellar flux from the disk surface. The midplane temperatures
in the shadowed part of the disk are governed by the
→ near infrared emission of the inner rim,
scattering of stellar light by dust particles outside the disk plane, and radial
diffusion which exchanges energy between adjacent slabs. Etymology (EN): Flared, from flare “to spread gradually outward, as the end of a trumpet, having a gradual increase in width,” of unknown origin; → disk. Etymology (PE): Gerdé, → disk; borun-gošâ “opening outward,” from borun “out, the outside” (Mid.Pers. bêron, from bê “outside, out, away” + rôn “side, direction;” Av. ravan- “(course of a) river”) + gošâ stem of gošâdan, gošudan “to open;” Mid.Pers. wišâdan “to open, let free;” Khotanese hiyā “bound;” O.Pers. višta “untied, loosend;” vištāspa- (personal name) “with loosened horses;” Av. višta “untied,” hita- “fastened, tied on;” cf. Skt. sā- “to bind, fasten,” syáti “binds.” |