The COMPLETE Survey of Outflows in Perseus
... the cloud. Perseus contains two rich protostellar clusters, IC 348 and NGC 1333, and a number of other regions of active star formation including B5, B1, L1448, and L1455 (see Figure 1). Surveys in the infrared, sub-millimeter, and millimeter reveal a large population of low-mass premain sequence st ...
... the cloud. Perseus contains two rich protostellar clusters, IC 348 and NGC 1333, and a number of other regions of active star formation including B5, B1, L1448, and L1455 (see Figure 1). Surveys in the infrared, sub-millimeter, and millimeter reveal a large population of low-mass premain sequence st ...
Evolution and fate of very massive stars
... (VMS) in the local universe. First, very massive stars (Mini . 320 M ) have been observed in the Large Magellanic Clouds (LMC). Second, there are observed SNe that bear the characteristics of Pair Creation Supernovae (PCSNe , also referred to as pair-instability SN) which have very massive stars as ...
... (VMS) in the local universe. First, very massive stars (Mini . 320 M ) have been observed in the Large Magellanic Clouds (LMC). Second, there are observed SNe that bear the characteristics of Pair Creation Supernovae (PCSNe , also referred to as pair-instability SN) which have very massive stars as ...
Paper 3 (pdf)
... the seminal “unified model” of Seyfert galaxies, a subset of AGN. Their paper has been cited in over 1000 papers in 20 years, over 5% of all papers ever written about AGN. Thus, the extra information from polarimetric observations has provided a fundamental contribution to the understanding of AGN. ...
... the seminal “unified model” of Seyfert galaxies, a subset of AGN. Their paper has been cited in over 1000 papers in 20 years, over 5% of all papers ever written about AGN. Thus, the extra information from polarimetric observations has provided a fundamental contribution to the understanding of AGN. ...
Hydrostatic equilibrium in a magnetized, warped Galactic disc
... regular and random magnetic fields contain disc and halo components, the parameters of which we have determined. The layer at 1 & |z| & 4 kpc can be overpressured and an outflow at a speed of about 50 km s21 may occur there, presumably associated with a Galactic fountain flow, if B0 . 2 mG. We show ...
... regular and random magnetic fields contain disc and halo components, the parameters of which we have determined. The layer at 1 & |z| & 4 kpc can be overpressured and an outflow at a speed of about 50 km s21 may occur there, presumably associated with a Galactic fountain flow, if B0 . 2 mG. We show ...
Chapter 10 Formation and evolution of the Local Group
... shows that almost all LG galaxies have RR Lyrae variables, suggestive of 10 Gyr old populations. As well he suggests that the oldest globular clusters formed out of halo gas shocked by ionization fronts generated during cosmic reionization at 5 < z < 15. Weinmann et al. (2007) studied the dependence ...
... shows that almost all LG galaxies have RR Lyrae variables, suggestive of 10 Gyr old populations. As well he suggests that the oldest globular clusters formed out of halo gas shocked by ionization fronts generated during cosmic reionization at 5 < z < 15. Weinmann et al. (2007) studied the dependence ...
3011800000631
... We have evaluated all available data, from the earlier observations in the optical and near infrared bands, and from the recent Spitzer observations in the mid-IR with gas disk models (Ertan et al. 2006). We find that the combined data set can be fit by a conventional gaseous disk model with viscous ...
... We have evaluated all available data, from the earlier observations in the optical and near infrared bands, and from the recent Spitzer observations in the mid-IR with gas disk models (Ertan et al. 2006). We find that the combined data set can be fit by a conventional gaseous disk model with viscous ...
Science performance of Gaia, ESA`s space
... Galaxy, including the build up of its different stellar components through past accretion and merger events with smaller satellite galaxies (Fig. 1). The distributions of stars in the Galaxy over position and velocity are linked through gravitational forces and the starformation rate and history as ...
... Galaxy, including the build up of its different stellar components through past accretion and merger events with smaller satellite galaxies (Fig. 1). The distributions of stars in the Galaxy over position and velocity are linked through gravitational forces and the starformation rate and history as ...
A magnetic communication scenario for hot Jupiters
... We obtain the best fits for the values for B and T that are listed together with the other (fixed) parameters in Table 1. They both appear to lie in the lower region of reasonable values, where we take the Solar values as an orientation. The parameter space leading to phase differences near the ob ...
... We obtain the best fits for the values for B and T that are listed together with the other (fixed) parameters in Table 1. They both appear to lie in the lower region of reasonable values, where we take the Solar values as an orientation. The parameter space leading to phase differences near the ob ...
Theoretical Predictions for Mass Loss Rates: Rotation & Pulsation
... • Acceleration thus depends on velocity & velocity gradient! This turns “F=ma” ...
... • Acceleration thus depends on velocity & velocity gradient! This turns “F=ma” ...
WIMPs and MACHOs - Caltech Astronomy
... couplings, so the distinction is especially important for dark matter detection efforts. For example, the WIMP class of particles can be defined as those particles that are created thermally, while dark matter axions come mostly from non-thermal processes. Light neutrinos are also thermally created ...
... couplings, so the distinction is especially important for dark matter detection efforts. For example, the WIMP class of particles can be defined as those particles that are created thermally, while dark matter axions come mostly from non-thermal processes. Light neutrinos are also thermally created ...
O stars with weak winds: the Galactic case - Max-Planck
... The instrumental resolution varies between 0.04 Å and 0.1 Å, due to different slit widths. The UVES pipeline was used for the reduction of the data. Second, optical data for HD 34078 and HD 15629 were retrieved from the La Palma archive. Spectra obtained with the instrument ISIS on the WHT were re ...
... The instrumental resolution varies between 0.04 Å and 0.1 Å, due to different slit widths. The UVES pipeline was used for the reduction of the data. Second, optical data for HD 34078 and HD 15629 were retrieved from the La Palma archive. Spectra obtained with the instrument ISIS on the WHT were re ...
Theoretical and observational framework Spectroscopic approach
... • The presence of fast HB rotators is confirmed and extended to other clusters. • The abundance of fast HB rotators can apparently change from cluster to cluster. • The change in rotational velocity seems to be associated to the onset of diffusive processes in the stellar atmosphere. • Radiative lev ...
... • The presence of fast HB rotators is confirmed and extended to other clusters. • The abundance of fast HB rotators can apparently change from cluster to cluster. • The change in rotational velocity seems to be associated to the onset of diffusive processes in the stellar atmosphere. • Radiative lev ...
FIVE NEW TRANSITS OF THE SUPER
... Many clues about the processes of planet formation and evolution have been discovered by studying the ensemble properties of exoplanets, such as the ‘‘brown dwarf desert’’ ( Halbwachs et al. 2000; Marcy & Butler 2000) and the tendency for metal-rich stars to have more detectable planets (Santos et a ...
... Many clues about the processes of planet formation and evolution have been discovered by studying the ensemble properties of exoplanets, such as the ‘‘brown dwarf desert’’ ( Halbwachs et al. 2000; Marcy & Butler 2000) and the tendency for metal-rich stars to have more detectable planets (Santos et a ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.