Mass Functions in Fractal Clouds: The Role of Cloud Structure in the
... There are many physical processes involved, and it is not generally clear which dominate the IMF. Moreover, the simulations differ from each other in the presence of magnetic forces, magnetic diffusion, turbulence driving, initial cloud boundedness, gas cooling, stellar outflows, starlight heating, ...
... There are many physical processes involved, and it is not generally clear which dominate the IMF. Moreover, the simulations differ from each other in the presence of magnetic forces, magnetic diffusion, turbulence driving, initial cloud boundedness, gas cooling, stellar outflows, starlight heating, ...
Absolute Flux Calibration
... most of the solar planets have strong mm-emission and reasonably well derived flux models • Contra: 1.) Fluxes not completely constant Mars 2.) They start to be resolved (≥ 3”) already at 3mm 3.) Some of them have broad molecular line absorption (e.g., Mars, Jupiter, Saturn) 4.) Not always visible, ...
... most of the solar planets have strong mm-emission and reasonably well derived flux models • Contra: 1.) Fluxes not completely constant Mars 2.) They start to be resolved (≥ 3”) already at 3mm 3.) Some of them have broad molecular line absorption (e.g., Mars, Jupiter, Saturn) 4.) Not always visible, ...
Proposal - ESA Science
... 10.5 Consortium Contributing Scientists & Engineers .............................................................. 57 10.6 Acknowledgements ................................................................................................. 59 ...
... 10.5 Consortium Contributing Scientists & Engineers .............................................................. 57 10.6 Acknowledgements ................................................................................................. 59 ...
Practical cosmology with the Local Volume galaxies
... dark matter distribution on scales of 0.3 – 3 Mpc. In this respect we note that the sum of virial mass for 7 nearest groups (around the Milky Way, M31, M81, CenA, M83, IC342, and Maffei) consists of 1.3·1013 M☼. But the sum of their total masses estimated via R0 from external galaxy motions is 0.86· ...
... dark matter distribution on scales of 0.3 – 3 Mpc. In this respect we note that the sum of virial mass for 7 nearest groups (around the Milky Way, M31, M81, CenA, M83, IC342, and Maffei) consists of 1.3·1013 M☼. But the sum of their total masses estimated via R0 from external galaxy motions is 0.86· ...
IRAM Annual Report 2012
... one of the key elementary bricks in the formation of complex organic molecules and in the emergence of life. According to current models of disk chemistry, HC3N is mainly formed through grain surface reactions in the colder regions (≤15 K) near the disk mid-plane. Contrary to HC3N, simple molecules ...
... one of the key elementary bricks in the formation of complex organic molecules and in the emergence of life. According to current models of disk chemistry, HC3N is mainly formed through grain surface reactions in the colder regions (≤15 K) near the disk mid-plane. Contrary to HC3N, simple molecules ...
Super-Earth and Sub-Neptune Exoplanets: a First Look from the
... Kepler satellite indicate that main-sequence stars on average host, at a minimum, about one planet per star (Fressin et al. 2013; Dressing & Charbonneau 2013). For the first time in human history, we have incontrovertible evidence that planets are common around other stars in the Milky Way. With thi ...
... Kepler satellite indicate that main-sequence stars on average host, at a minimum, about one planet per star (Fressin et al. 2013; Dressing & Charbonneau 2013). For the first time in human history, we have incontrovertible evidence that planets are common around other stars in the Milky Way. With thi ...
Chap2-RadialVelocity
... Wavelength calibration Wavelength calibration is key for achieving accurate Doppler measurements. It is certainly one of the most important design drivers of modern precision radial velocity (PRV) instruments. ...
... Wavelength calibration Wavelength calibration is key for achieving accurate Doppler measurements. It is certainly one of the most important design drivers of modern precision radial velocity (PRV) instruments. ...
Structure of Hot Molecular Cores
... 3.6.1 Temperature computation . . . . . . . . . . . . 3.6.2 A grid of models . . . . . . . . . . . . . . . . . 3.6.3 Selection . . . . . . . . . . . . . . . . . . . . . 3.7 Modeling procedure: Lines . . . . . . . . . . . . . . . . 3.7.1 Line radiative transfer . . . . . . . . . . . . . . 3.7.2 Fitti ...
... 3.6.1 Temperature computation . . . . . . . . . . . . 3.6.2 A grid of models . . . . . . . . . . . . . . . . . 3.6.3 Selection . . . . . . . . . . . . . . . . . . . . . 3.7 Modeling procedure: Lines . . . . . . . . . . . . . . . . 3.7.1 Line radiative transfer . . . . . . . . . . . . . . 3.7.2 Fitti ...
Abstract The Star Formation History of Low Surface Brightness Galaxies
... impression that they may simply be faded remnants of higher surface brightness galaxies whose star formation has finished. Other scenarios span a broad range: a young mean age, less dust, a lower metallicity, perhaps even a variable IMF. Distinguishing between these scenarios requires sufficient inf ...
... impression that they may simply be faded remnants of higher surface brightness galaxies whose star formation has finished. Other scenarios span a broad range: a young mean age, less dust, a lower metallicity, perhaps even a variable IMF. Distinguishing between these scenarios requires sufficient inf ...
Tidal Effects on the Oort Cloud Comets and Dynamics of the Sun in
... The Solar System presents a complex dynamical structure and is not isolated from the Galaxy. In particular the comet reservoir of our planetary system, the Oort cloud, is extremely sensitive to the the galactic environment due to its peripheral collocation inside the Solar System. In this framework, ...
... The Solar System presents a complex dynamical structure and is not isolated from the Galaxy. In particular the comet reservoir of our planetary system, the Oort cloud, is extremely sensitive to the the galactic environment due to its peripheral collocation inside the Solar System. In this framework, ...
PPT - University of Waterloo
... Formation and evolution of galaxies and clusters in the early universe Star formation rates, bolometric luminosities, AGN structure Evolution of chemical elements Formation of stars & planets and physics of the interstellar medium Tracers of structure, kinematics, chemistry in star forming reg ...
... Formation and evolution of galaxies and clusters in the early universe Star formation rates, bolometric luminosities, AGN structure Evolution of chemical elements Formation of stars & planets and physics of the interstellar medium Tracers of structure, kinematics, chemistry in star forming reg ...
Andrea Santangelo
... • How the energy of the line is related to the luminosity ? Do we observe a change of regime ...
... • How the energy of the line is related to the luminosity ? Do we observe a change of regime ...
ASI 2017 Abstract Book - Astronomical Society of India
... One of the most outstanding challenges in extragalactic astronomy is to identify the astrophysical processes responsible for transforming simple dark matter haloes into the heterogenous population of galaxies inhabiting today's Universe. How did different morphological types form and evolve? Does th ...
... One of the most outstanding challenges in extragalactic astronomy is to identify the astrophysical processes responsible for transforming simple dark matter haloes into the heterogenous population of galaxies inhabiting today's Universe. How did different morphological types form and evolve? Does th ...
Ages of young stars
... are combinations of theoretical uncertainties and observational uncertainties associated with estimating the luminosity of the LDB. Contributing to the latter are distance estimates, reddening and bolometric corrections (for stellar luminosity not in the band observed), but these are usually small c ...
... are combinations of theoretical uncertainties and observational uncertainties associated with estimating the luminosity of the LDB. Contributing to the latter are distance estimates, reddening and bolometric corrections (for stellar luminosity not in the band observed), but these are usually small c ...