Formation and evolution of giant molecular clouds in a barred spiral
... Understanding where and how gas is converted into stars in a galaxy is important for understanding a galaxy’s formation and evolution through each epoch of the universe. Which physical processes control the star formation in a galaxy is heavily debated. We are now at a stage where it is possible to ...
... Understanding where and how gas is converted into stars in a galaxy is important for understanding a galaxy’s formation and evolution through each epoch of the universe. Which physical processes control the star formation in a galaxy is heavily debated. We are now at a stage where it is possible to ...
The 3-D shaping of NGC 6741: A massive, fast
... photo-ionization model, spatial structure and evolutionary phase of the Planetary Nebula NGC 6741 by means of long-slit ESO NTT+EMMI high-resolution spectra at nine position angles, reduced and analysed according to the tomographic and 3-D methodologies developed at the Astronomical Observatory of P ...
... photo-ionization model, spatial structure and evolutionary phase of the Planetary Nebula NGC 6741 by means of long-slit ESO NTT+EMMI high-resolution spectra at nine position angles, reduced and analysed according to the tomographic and 3-D methodologies developed at the Astronomical Observatory of P ...
Lithium abundances in nearby FGK dwarf and subgiant stars
... therefore having an important impact on rotational mixing (e.g., Bouvier 2008). In both cases, enhanced lithium depletion is expected for stars hosting planets. Lithium abundances in stellar photospheres could, therefore, be of interest also for exoplanet research. However, sample biases must be cle ...
... therefore having an important impact on rotational mixing (e.g., Bouvier 2008). In both cases, enhanced lithium depletion is expected for stars hosting planets. Lithium abundances in stellar photospheres could, therefore, be of interest also for exoplanet research. However, sample biases must be cle ...
Chapter 5 Thin Accretion Disks
... If Re1, viscous force dominates the flow; if Re1, the viscosity is dynamically unimportant. In the case of molecular viscosity due to Coulomb collisions between charged particles in the ionized gas, given by d and v ~ cs, ...
... If Re1, viscous force dominates the flow; if Re1, the viscosity is dynamically unimportant. In the case of molecular viscosity due to Coulomb collisions between charged particles in the ionized gas, given by d and v ~ cs, ...
arXiv:1410.8731v2 [astro
... We analyse and report in detail new near-infrared (1.45 - 2.45 microns) observations of the Dusty S-cluster Object (DSO/G2) during its approach to the black hole at the center of the Galaxy that were carried out with ESO VLT/SINFONI between February and September 2014. Before May 2014 we detect spat ...
... We analyse and report in detail new near-infrared (1.45 - 2.45 microns) observations of the Dusty S-cluster Object (DSO/G2) during its approach to the black hole at the center of the Galaxy that were carried out with ESO VLT/SINFONI between February and September 2014. Before May 2014 we detect spat ...
Th`ese d`astrophysique Chemodynamical Simulations of Evolution
... Interstellar extinction in UV has a bump located at 2,200 Å, explained with presence of grains by Seaton (1979). Savage & Mathis (1979) is an early review on properties of dust. Mathis et al. (1977) have studied extinction from ultraviolet to infrared to conclude on a power law for size distributio ...
... Interstellar extinction in UV has a bump located at 2,200 Å, explained with presence of grains by Seaton (1979). Savage & Mathis (1979) is an early review on properties of dust. Mathis et al. (1977) have studied extinction from ultraviolet to infrared to conclude on a power law for size distributio ...
Fundamental properties of Ana González Galán
... The aim of this thesis is to characterise a sample of High Mass X-ray Binaries (HMXBs) formed by: IGR J00370+6122, XTE J1855-026, AX J1841.0-0535 and AX J1845.0-0433. These objects are composed of pulsars (rotating neutron stars) accreting material from the wind of their supergiant companions. The X ...
... The aim of this thesis is to characterise a sample of High Mass X-ray Binaries (HMXBs) formed by: IGR J00370+6122, XTE J1855-026, AX J1841.0-0535 and AX J1845.0-0433. These objects are composed of pulsars (rotating neutron stars) accreting material from the wind of their supergiant companions. The X ...
The Relation between Interstellar Turbulence and Star Formation
... Accretion onto these objects will vary with time and depend on the properties of the surrounding turbulent flow. This has important consequences for the resulting stellar mass function. Star formation on scales of galaxies as a whole is expected to be controlled by the balance between gravity and tu ...
... Accretion onto these objects will vary with time and depend on the properties of the surrounding turbulent flow. This has important consequences for the resulting stellar mass function. Star formation on scales of galaxies as a whole is expected to be controlled by the balance between gravity and tu ...
Oxygen, magnesium and chromium isotopic ratios of
... as well as excesses and deficits in 25Mg. We present the results of new model calculations of the evolution of Mg and Al isotopic ratios in the envelopes of AGB stars for a range of masses (1.5, 2, 3, and 5 MJ), metallicities (1/6, 1/3, 1/2 and 1ZJ) and different prescriptions for mass loss by stell ...
... as well as excesses and deficits in 25Mg. We present the results of new model calculations of the evolution of Mg and Al isotopic ratios in the envelopes of AGB stars for a range of masses (1.5, 2, 3, and 5 MJ), metallicities (1/6, 1/3, 1/2 and 1ZJ) and different prescriptions for mass loss by stell ...
2004 Report on Research Activities 2003
... beta ray spectrometers with the aim to study excited levels of neutron-deficient isotopes provided by the 660 MeV cyclotron of the Joint Institute for Nuclear Research in Dubna. In parallel, studies of spin polarization of neutrons and protons emitted in the deuteron stripping reaction were performe ...
... beta ray spectrometers with the aim to study excited levels of neutron-deficient isotopes provided by the 660 MeV cyclotron of the Joint Institute for Nuclear Research in Dubna. In parallel, studies of spin polarization of neutrons and protons emitted in the deuteron stripping reaction were performe ...
ROSAT Isolated Neutron Stars
... Basics Compact objects are born in the core collapse following a type II supernova explosion Present rate of SN events in the Galaxy: ≈ 0.01/yr (possibly higher in the past) Galactic population of compact objects: ≈ 108 – 109 (≈ 1% of stars) ...
... Basics Compact objects are born in the core collapse following a type II supernova explosion Present rate of SN events in the Galaxy: ≈ 0.01/yr (possibly higher in the past) Galactic population of compact objects: ≈ 108 – 109 (≈ 1% of stars) ...
ULTRA-COMPACT HII REGIONS AND MASSIVE STAR FORMATION
... when resolved. This observationally based definition of HCs is broad enough to apply to any hot, dust/molecular gas–enshrouded object such as UC HII regions, evolved hot stars that have moved into a dense molecular cloud, or massive protostars still undergoing rapid accretion. In this section, I con ...
... when resolved. This observationally based definition of HCs is broad enough to apply to any hot, dust/molecular gas–enshrouded object such as UC HII regions, evolved hot stars that have moved into a dense molecular cloud, or massive protostars still undergoing rapid accretion. In this section, I con ...
UCNSD2v12 - Experimental Subatomic Physics
... 0.1% or better. This would allow a determination of GA and GV solely within the neutron system with an accuracy better than any other technique. In particular, this would avoid the problems associated with Coulomb effects and radiative corrections that must be applied to the 0+ 0+ nuclear beta dec ...
... 0.1% or better. This would allow a determination of GA and GV solely within the neutron system with an accuracy better than any other technique. In particular, this would avoid the problems associated with Coulomb effects and radiative corrections that must be applied to the 0+ 0+ nuclear beta dec ...
The white dwarf luminosity function
... White dwarfs are the final evolutionary stage of stars with masses less than 10±2 M⊙ , though the upper mass limit is not yet well known (Ritossa et al., 1999). Van Dyk et al. (2003), Smartt et al. (2004), Maund et al. (2005) and Li et al. (2006) attempted to provide observational limits on the maxi ...
... White dwarfs are the final evolutionary stage of stars with masses less than 10±2 M⊙ , though the upper mass limit is not yet well known (Ritossa et al., 1999). Van Dyk et al. (2003), Smartt et al. (2004), Maund et al. (2005) and Li et al. (2006) attempted to provide observational limits on the maxi ...
Accretion Power in Astrophysics, Third Editiion
... in an appendix. The astrophysics of stellar accretion is dealt with in Chapters 4 to 6. Chapters 7 and 8 set the observational scene for two models of active nuclei (or possibly for two aspects of a single model) considered in Chapters 9 and 10. In the main we have not given references to sources, s ...
... in an appendix. The astrophysics of stellar accretion is dealt with in Chapters 4 to 6. Chapters 7 and 8 set the observational scene for two models of active nuclei (or possibly for two aspects of a single model) considered in Chapters 9 and 10. In the main we have not given references to sources, s ...
Evidence of suppression of star formation by quasar
... tribution of galaxy colors. If AGN feedback couples to the gas as efficiently as required by galaxy formation models, then massive, early-type galaxies will be gas-poor and passively aging, while younger galaxies, typically lower-mass, late-type galaxies will still have enough star formation materia ...
... tribution of galaxy colors. If AGN feedback couples to the gas as efficiently as required by galaxy formation models, then massive, early-type galaxies will be gas-poor and passively aging, while younger galaxies, typically lower-mass, late-type galaxies will still have enough star formation materia ...
Post-starburst galaxies: more than just an interesting curiosity
... 1997; Noeske et al. 2007; Tresse et al. 2007). However, the process, or processes, responsible for this gradual decline remain to be determined. What physical mechanisms cause a galaxy to stop forming stars, to turn into a spheroid, and thus to enter the red sequence? There are many competing theori ...
... 1997; Noeske et al. 2007; Tresse et al. 2007). However, the process, or processes, responsible for this gradual decline remain to be determined. What physical mechanisms cause a galaxy to stop forming stars, to turn into a spheroid, and thus to enter the red sequence? There are many competing theori ...
Giant Low Surface Brightness Galaxies
... Although they fall in the class of late type spiral galaxies, their properties are far more extreme. They have very faint stellar disks that are extremely rich in neutral hydrogen gas but low in star formation and hence low in surface brightness. They often have bright bulges that are similar to tho ...
... Although they fall in the class of late type spiral galaxies, their properties are far more extreme. They have very faint stellar disks that are extremely rich in neutral hydrogen gas but low in star formation and hence low in surface brightness. They often have bright bulges that are similar to tho ...
Co-production of Nitrogen-15 and Oxygen-18 in
... 4 times the solar value in the green perimeter while the δ 18 O/16 O value peaks at 5200 parts per mil in the two red spots, corresponding to ...
... 4 times the solar value in the green perimeter while the δ 18 O/16 O value peaks at 5200 parts per mil in the two red spots, corresponding to ...
Envelope inflation in massive stars near the Eddington limit
... Man’s fascination with stars began many centuries ago. From ancient times, people across multiple cultures, from the Aztecs in America to the Hindus in modern day India, have worshipped the Sun, the nearest star and the source of life on earth. Apart from having deep-rooted cultural significance, as ...
... Man’s fascination with stars began many centuries ago. From ancient times, people across multiple cultures, from the Aztecs in America to the Hindus in modern day India, have worshipped the Sun, the nearest star and the source of life on earth. Apart from having deep-rooted cultural significance, as ...
CENTRAL STARS OF PLANETARY NEBULAE IN THE LARGE
... central star of the PN (CSPN), and the size and ionized mass of the PN itself. This obstruction is removed for the PNe of the LMC, all of which lie at essentially the same distance, allowing the physical parameters to be scaled to absolute values. In addition, the lower metallicity of the LMC relati ...
... central star of the PN (CSPN), and the size and ionized mass of the PN itself. This obstruction is removed for the PNe of the LMC, all of which lie at essentially the same distance, allowing the physical parameters to be scaled to absolute values. In addition, the lower metallicity of the LMC relati ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.