[PDF] Top 20 Dust formation in the oxygen-rich AGB star IK Tauri

... formed dust grains in the gas and derive a mass loss for IK ...cluster formation and dust condensation in the inner ...the dust radiative feedback on the gas ...of AGB winds, ... See full document

... of dust condensation in the outflow from oxygen-rich AGB stars is a continuing ...the formation of gas- phase precursors from Ca, Mg, Fe, SiO and TiO in an outflow cooling from 1500 to ... See full document

... of AGB stars get progressively more carbon-rich. Therefore oxygen-rich AGB stars can have carbon-to- oxygen ratios (C/O) ranging from cosmic, ∼ ...remain ... See full document

... branch. Dust-driven winds (radiation pressure due to large luminosities) then enrich the ISM with these ele- ...solar-metallicity AGB stars with C / O∼1, and a C / O>2 are considered ...low-metallicity ... See full document

... (PMS) star ap- proaches its final mass, the envelope starts to become optically thin at infrared ...T Tauri and Herbig Ae/Be stars, HST observations laid all doubts to rest by imaging the scattered light ... See full document

... There remain many unanswered questions in the field of red giant and cool star research, many of which apply to the Sun itself. How do rotation and convection combine to drive the dynamo process, which is thought ... See full document

... Notice that we assume the gas layer only has one temperature, as we assume LTE. But we know this may not necessarily be the case. So in reality, most likely, the gas layer will have more than one temperature, (or have ... See full document

... Thus far, numerous photometric studies on the variability of YSOs have been conducted. In [5], the photometric monitoring of 24 YSOs was reported, and the authors observed one or two (quasi-) sinusoidal curve(s) with a ... See full document

... in star spot coverage (or limb-darkening, though with heavy spot coverage, the two effects become some- what ...the star and the extreme proximity of the companion, such features may be compounded by ... See full document

... AKARI FIS bands. Hirashita et al. (2008) proposed a for- mula to estimate the TIR luminosity at λ = 3–1000 μm using the flux densities of three AKARI bands: N60, WIDE- S, and WIDE-L, for the AKARI pointed observation ... See full document

... between dust and gas in local galaxies, which allows estimates of the gas mass to be obtained very quickly via observations of the Rayleigh-Jeans continuum (see Scoville et ... See full document

... of dust and stars in shaping the gradi- ...the dust-mass surface density are larger than those of the surface-brightness profiles at 500 µm, generally larger than any of the other surface-brightness ... See full document

... will grow only by ∼ 0.2 dex to z = 0. While this is still enough fractional growth (∼ 50%) to make the galaxy blue, if all the newly accreted gas were to cool immediately and form new stars, it is unlikely that this ... See full document

... Taurus L1495 filamentary complex [7]. Because this core is very dense, with a high deu- terium fraction it indicates that it should be at the very end of its starless phase. Hence, it may be the precursor of a brown ... See full document

... models. For the PP case, we consider photons from the radial direction only but the full shielding (dust + self- + H + H 2 ) was included. The envelope was illuminated by a Draine (1978) field, extended to ... See full document

... stripped off by the RLOF, and the naked helium core (with a thin hydrogen envelope) gets ignited to produce a hot subdwarf star. In the CE ejection channel, the mass donor fills its Roche lobe near the tip of the ... See full document

... superposition. If rounded to the nearest 10 s, the standard deviation of the H  smoothed_ K CCF does not reach 530 s ( the next possible value broader than that of the original H K  ) until K is averaged over a window ... See full document

... Figure 4. Position–velocity diagram for our selected galaxies extracted along the major axis. Contour levels are evenly spaced between three times the rms level to the peak flux in nine increments. The majority of the ... See full document

... and dust particles), when combined, increase their mass (the mass of particles of the dust subsystem is constantly growing), ...and dust particles arriving from more distant radial distances ... See full document

... characteristic dust temper- ature roughly corresponds to the wavelength at which a galaxy’s SED ...warmer dust temperatures, or equivalently their dust SEDs peak at shorter wavelengths, at fixed ... See full document