[PDF] Top 20 The environments in which stars and circumstellar discs form

... (2002) which require inwardly migrating dust slowed by P-R drag to get caught in the planet’s resonances which as discussed earlier may be removed from the system by the action of collisions and radiation ... See full document

... Be stars are found in both lower- and higher-metallicity environments, with lower metallicity showing higher prevalence of the Be phenomenon (Martayan, Baade, and Fabregat, 2010; McSwain and Gies, 2005), we ... See full document

... here, which includes the simulated stellar winds and inner astrospheres of the systems of ...planet, which interacts self-consistently with the incident stellar ...these stars are calculated, ... See full document

... photodissociation is sufficiently large, the atmosphere can be pushed out of thermochemical equilib- rium (see, e.g., Moses, 2014; Miguel & Kaltenegger, 2014; Hu & Seager, 2014). This effect has been observed in ... See full document

... Figure 6.18 presents the BAAVSS observations of this star (both filtered and unfiltered) made during 1988-1990. It appears th a t there are system atic differences between observers for this star, w ith m agnitude estim ... See full document

... stars, including PNs in the Milky Way and the Magellanic Clouds, a protoplanetary nebula (PPN), post asymptotic gi- ant branch (AGB) stars, modestly hydrogen-deficient RCB stars, and a peculiar binary ... See full document

... Although the molecular composition of the CSE of SMP LMC 11 is certainly unique thus far, we do not believe that the environment represented by this object is necessarily excep- tional. CRL 618 is the only other source ... See full document

... low-mass stars in the solar neighbourhood ...massive stars available in young GCs to provide enriched ...to discs from the surrounding material is expected to be orders of magnitude higher than in ... See full document

... the environments of the ONC and NGC 2024 are similar, they are different from that of USco in that USco is a low stellar-density, OB association rather than a high stellar-density embedded ...common which IC ... See full document

... protoplanetary discs have mostly used direct imaging and this is one of the first using radial velocity to probe a parameter space not accessible by photometry: closer binaries with periods < 20 ...of ... See full document

... Protoplanetary discs – discs of gas and dust that surround young pre-main-sequence stars – are the birthplaces of ...of discs. Protoplane- tary discs consist of gas and ... See full document

... towards circumstellar discs that are present at very small scales, the logical, direct conclusion we can draw is that the disk is not truncated, but reaches all the way down to the stellar ...massive ... See full document

... debris discs around main-sequence A-type ...with which to investigate the cold disc ...A stars yields a lower than previously found debris disc ...m which is similar to the debris disc rate ... See full document

... trunk discs, then branch like fingers of a glove, and that the nephridiopores develop after ...organ discs and the larval stomach), but interpreted them as being derived from the subumbrellar epidermis near ... See full document

... regarding the dense gas near x ∼ 0.05 pc and z ∼ 0: As the magnetic field strength is increased, this clump becomes more compact and denser. However, this trend is broken by N03, in which this clump does not ... See full document

... Another important aim of this thesis is to compare the results of the 1992 international observing campaign with the more extensive data set contained in this thesis, from MJUO. The results of the 1992 campaign ... See full document

... in which evolutionary phases massive stars form their circumstellar nebu- ...could form around red supergiants (Mackey et al. 2014), which unlike the shells around Wolf–Rayet ... See full document

... the heliocentric velocity frame. These features are too narrow to be photospheric in nature and therefore they must be produced by absorption of stellar light by either an IS or circumstellar gas cloud. There is a ... See full document

... the stars polarise the continuum photons while the emission photons are ...some stars the lines are so faint that the emission does not even reach the photospheric ... See full document

... chemistry in the outer CSE. This influence has two observable aspects: one leads to changes in the radial distribution of the species’ peak abundances. These distributions will become in- creasingly observable after ... See full document