FIELD GALAXIES AND THEIR AGNs: NATURE VERSUS
... Dark matter halos are the only objects forming as long as the gas is ionized. Formation of the first ”baryon objects” or proto-galaxies is much more complicated. The exact physics of galaxy formation depends on which process is dominant (star formation, mechanical and radiative physics, turbulence, ...
... Dark matter halos are the only objects forming as long as the gas is ionized. Formation of the first ”baryon objects” or proto-galaxies is much more complicated. The exact physics of galaxy formation depends on which process is dominant (star formation, mechanical and radiative physics, turbulence, ...
Studies of dark matter in and around stars
... in every day life. The gravitational effects of this dark matter have been observed in many different ways but its true nature is still unknown. In most models, dark matter particles can annihilate with each other into standard model particles; the direct or indirect observation of such annihilation ...
... in every day life. The gravitational effects of this dark matter have been observed in many different ways but its true nature is still unknown. In most models, dark matter particles can annihilate with each other into standard model particles; the direct or indirect observation of such annihilation ...
Gamma-Ray Bursts and Puzzles of Core
... These are spectra with the high S/N ratio. The 6100A absorption (trough) reaches the maximal depth and width at the moment UT Feb ~ 23. Here we do not take into account the early spectrum of their paper Modjaz et al. (0603377), obtained with the low S/N ratio at the FLWO 1.5m telescope 3.97 days aft ...
... These are spectra with the high S/N ratio. The 6100A absorption (trough) reaches the maximal depth and width at the moment UT Feb ~ 23. Here we do not take into account the early spectrum of their paper Modjaz et al. (0603377), obtained with the low S/N ratio at the FLWO 1.5m telescope 3.97 days aft ...
PPT presentation
... samples of PN radial velocities are reaching the precision which will allow to discriminate the efficiency of the baryon cooling in galaxies. We have shown on a sample of 21 galaxies that the M/L gradients by PN and stellar kinematics are generally in agreement with the LCDM expectations with some “ ...
... samples of PN radial velocities are reaching the precision which will allow to discriminate the efficiency of the baryon cooling in galaxies. We have shown on a sample of 21 galaxies that the M/L gradients by PN and stellar kinematics are generally in agreement with the LCDM expectations with some “ ...
The Secular and Rotational Brightness Variations of Neptune
... transformations but all the data analyzed here have been transformed. Formal errors are not available for these observations though they are estimated to be a few hundredths of a magnitude or less based on scatter in the data obtained over short periods of time as well as the likely uncertainties in ...
... transformations but all the data analyzed here have been transformed. Formal errors are not available for these observations though they are estimated to be a few hundredths of a magnitude or less based on scatter in the data obtained over short periods of time as well as the likely uncertainties in ...
X-ray astronomy of stellar coronae (Review)
... 11-year magnetic spot cycle, Fig. 1), but this effect is not directly dependent on the rotation period. Conversely, the well-studied solar activity cycle motivates us to investigate similar magnetic modulations in stars in order to confine the underlying dynamo mechanism. Stars allow us to study lon ...
... 11-year magnetic spot cycle, Fig. 1), but this effect is not directly dependent on the rotation period. Conversely, the well-studied solar activity cycle motivates us to investigate similar magnetic modulations in stars in order to confine the underlying dynamo mechanism. Stars allow us to study lon ...
Lecture 2
... • LBGs at z=3 and below are selected in the UGR colour-colour plane • They are very faint compared to local galaxies => difficult to observe • These galaxies have been followed up in great detail and their properties are now well understood • These properties include stellar ages, ...
... • LBGs at z=3 and below are selected in the UGR colour-colour plane • They are very faint compared to local galaxies => difficult to observe • These galaxies have been followed up in great detail and their properties are now well understood • These properties include stellar ages, ...
ALMA - National Radio Astronomy Observatory
... make detailed images of astronomical objects. The scope of the ALMA Project is an array of 64 antennas that can be positioned as needed over an area up to 14 kilometers in diameter so as to give the array a zoom-lens capability, with resolution reaching 10 milliarcseconds. The faintest millimeter/su ...
... make detailed images of astronomical objects. The scope of the ALMA Project is an array of 64 antennas that can be positioned as needed over an area up to 14 kilometers in diameter so as to give the array a zoom-lens capability, with resolution reaching 10 milliarcseconds. The faintest millimeter/su ...
The physics of line-driven winds of hot massive stars
... Galaxies are comprised of stars and clouds of gas. Stars that appear equally bright to the naked eye may either be nearby objects that are relatively dim or distant objects that are very luminous. The intrinsically brightest stars are the topic of this thesis. Their luminosities can be more than a m ...
... Galaxies are comprised of stars and clouds of gas. Stars that appear equally bright to the naked eye may either be nearby objects that are relatively dim or distant objects that are very luminous. The intrinsically brightest stars are the topic of this thesis. Their luminosities can be more than a m ...
Galaxies
... model of galaxy evolution and cosmology based on the paradigm that galaxies form hierarchically around peaks in the dark matter density distribution. Within this framework, astronomers have made great progress in understanding the large-scale clustering of galaxies, as biased tracers of the underlyi ...
... model of galaxy evolution and cosmology based on the paradigm that galaxies form hierarchically around peaks in the dark matter density distribution. Within this framework, astronomers have made great progress in understanding the large-scale clustering of galaxies, as biased tracers of the underlyi ...
Published in Contemp. Phys. 51, 464-465 (2010).
... it will fade until, in ∼210,000 years time, it will relinquish its title as our brightest star. Sirius would have passed right across the Milky Way during the stone age. One of the Arabic names for Sirius is al-schira al-abur, or “Sirius which has passed across”, raising the fascinating speculation ...
... it will fade until, in ∼210,000 years time, it will relinquish its title as our brightest star. Sirius would have passed right across the Milky Way during the stone age. One of the Arabic names for Sirius is al-schira al-abur, or “Sirius which has passed across”, raising the fascinating speculation ...
submillimeter observations of giant molecular clouds in the large
... with significantly better quality than before in terms of noise level, as well as angular resolution. It is also noteworthy that the current frequency coverage extends as high as the 800 GHz band and even the terahertz region. Among nearby galaxies that we can observe at reasonably high spatial reso ...
... with significantly better quality than before in terms of noise level, as well as angular resolution. It is also noteworthy that the current frequency coverage extends as high as the 800 GHz band and even the terahertz region. Among nearby galaxies that we can observe at reasonably high spatial reso ...
What is the real nature of HD 108?
... near λλ 4485, 4504 are also present. All Balmer lines except Hα appear as P Cygni profiles during most of our observing runs, but their morphology changes with time (see Sect. 6). On the contrary, some lines always appear in absorption, for example Si iv λλ 4088, 4116 and He ii λλ 4200, 4542. Some i ...
... near λλ 4485, 4504 are also present. All Balmer lines except Hα appear as P Cygni profiles during most of our observing runs, but their morphology changes with time (see Sect. 6). On the contrary, some lines always appear in absorption, for example Si iv λλ 4088, 4116 and He ii λλ 4200, 4542. Some i ...
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.