MUSE three-dimensional spectroscopy and kinematics of the
... Morganti et al. 1997). It is now considered they are young sources, forming part of an evolutionary sequence (An & Baan 2012; KunertBajraszewska 2015), which begins with high-frequency peaked sources, with few parsec diameters and low-frequency turnover at several GHz. These rapidly expand and incre ...
... Morganti et al. 1997). It is now considered they are young sources, forming part of an evolutionary sequence (An & Baan 2012; KunertBajraszewska 2015), which begins with high-frequency peaked sources, with few parsec diameters and low-frequency turnover at several GHz. These rapidly expand and incre ...
Planet transit and stellar granulation detection with interferometry
... ranging from optical to infrared. We chose an arbitrary date and arbitrary star with coordinates, and this ensures observability throughout the night. This optimisation of observability allows for a broad coverage of spatial frequencies. The stellar surface asymmetries in the brightness distribution ...
... ranging from optical to infrared. We chose an arbitrary date and arbitrary star with coordinates, and this ensures observability throughout the night. This optimisation of observability allows for a broad coverage of spatial frequencies. The stellar surface asymmetries in the brightness distribution ...
GammaRay Bursts, the Strongest Explosions in the Universe.
... Paczynski, Ramesh Narayan (from Harvard) I18 suggested internal shocks within the outflow as an alternative way to convert the kinetic energy to radiation. The basic idea was the collisionless shocks accelerate electrons and produce magnetic fields. The electrons movi ...
... Paczynski, Ramesh Narayan (from Harvard) I18 suggested internal shocks within the outflow as an alternative way to convert the kinetic energy to radiation. The basic idea was the collisionless shocks accelerate electrons and produce magnetic fields. The electrons movi ...
LARGE-SCALE EXTENDED EMISSION AROUND THE HELIX
... We present new observations of the ionized gas, molecular gas, and cool dust in the Helix Nebula (NGC 7293). The ionized gas is observed in the form of an H image, which is constructed using images from the Southern H Sky Survey Atlas. The molecular emission was mapped using the H2 v = 1 ! 0 S(1) ...
... We present new observations of the ionized gas, molecular gas, and cool dust in the Helix Nebula (NGC 7293). The ionized gas is observed in the form of an H image, which is constructed using images from the Southern H Sky Survey Atlas. The molecular emission was mapped using the H2 v = 1 ! 0 S(1) ...
Chapter 15 Stars, Galaxies and Universe
... The Big Bang Theory, continued • The big bang theory is the theory that all matter and energy in the universe was compressed into an extremely small volume that about 14 billion years ago exploded and began expanding in all directions. • Scientists believe that radio “noise” coming from all directio ...
... The Big Bang Theory, continued • The big bang theory is the theory that all matter and energy in the universe was compressed into an extremely small volume that about 14 billion years ago exploded and began expanding in all directions. • Scientists believe that radio “noise” coming from all directio ...
Unlocking the secrets of stellar haloes using combined star counts
... also show that while the haloes of these discs have extremely red colours, the discs themselves do not display any anomalous colours at the corresponding surface brightness levels. This strongly argues against a sky flux residual as the main culprit, since this would result in strange colours in bot ...
... also show that while the haloes of these discs have extremely red colours, the discs themselves do not display any anomalous colours at the corresponding surface brightness levels. This strongly argues against a sky flux residual as the main culprit, since this would result in strange colours in bot ...
the reality of the wolf 630 moving group - TigerPrints
... the efficient evaporation of younger clusters (i.e. interactions with giant molecular clouds Spitzer (1958)): they must either be formed outside of the disk or dynamically evolve there through some form of non-disruptive heating. Clearly open clusters, both young and old, are valuable targets in pie ...
... the efficient evaporation of younger clusters (i.e. interactions with giant molecular clouds Spitzer (1958)): they must either be formed outside of the disk or dynamically evolve there through some form of non-disruptive heating. Clearly open clusters, both young and old, are valuable targets in pie ...
IRC −10414: a bow-shock-producing red supergiant star
... Most runaway OB stars, like the majority of massive stars residing in their parent clusters, go through the red supergiant (RSG) phase during their lifetimes. Nonetheless, although many dozens of massive runaways were found to be associated with bow shocks, only two RSG bow-shock-producing stars, Be ...
... Most runaway OB stars, like the majority of massive stars residing in their parent clusters, go through the red supergiant (RSG) phase during their lifetimes. Nonetheless, although many dozens of massive runaways were found to be associated with bow shocks, only two RSG bow-shock-producing stars, Be ...
The colour–magnitude relation of early
... with those of F98, again with jDzj , 0:1. So-called catastrophic redshift errors can occur when the spectra of the model templates are a poor match to the observed colours (Yee 1998; Kodama et al. 1999), which happens predominantly with star-forming late-type galaxy spectra. In this analysis, we exp ...
... with those of F98, again with jDzj , 0:1. So-called catastrophic redshift errors can occur when the spectra of the model templates are a poor match to the observed colours (Yee 1998; Kodama et al. 1999), which happens predominantly with star-forming late-type galaxy spectra. In this analysis, we exp ...
Where is the angular momentum in elliptical galaxies?
... (to first order), so determining their age and metallicity is much simpler than for the composite populations in integrated light. • GCs are observed to form in all major star formation events in galaxies. • GCs are found out to very large radii around galaxies – useful dynamical probes of galaxy ha ...
... (to first order), so determining their age and metallicity is much simpler than for the composite populations in integrated light. • GCs are observed to form in all major star formation events in galaxies. • GCs are found out to very large radii around galaxies – useful dynamical probes of galaxy ha ...
Chapter 30 - Todd County Schools
... • A protostar’s temperature continually increases until it reaches about 10,000,000°C. • At this temperature, nuclear fusion begins. Nuclear fusion is a process in which less-massive atomic nuclei combine to form more-massive nuclei. The process releases enormous amounts of energy. • The onset of nu ...
... • A protostar’s temperature continually increases until it reaches about 10,000,000°C. • At this temperature, nuclear fusion begins. Nuclear fusion is a process in which less-massive atomic nuclei combine to form more-massive nuclei. The process releases enormous amounts of energy. • The onset of nu ...
Standardized Test Prep Chapter 30 Multiple Choice, continued
... • A protostar’s temperature continually increases until it reaches about 10,000,000°C. • At this temperature, nuclear fusion begins. Nuclear fusion is a process in which less-massive atomic nuclei combine to form more-massive nuclei. The process releases enormous amounts of energy. • The onset of nu ...
... • A protostar’s temperature continually increases until it reaches about 10,000,000°C. • At this temperature, nuclear fusion begins. Nuclear fusion is a process in which less-massive atomic nuclei combine to form more-massive nuclei. The process releases enormous amounts of energy. • The onset of nu ...
Stargazing For Beginners: A Binocular Tour of the Southern Night Sky
... visible from the Southern Hemisphere, along with dozens of deep-sky sights of interest within each constellation, such as galaxies, binary stars, nebulae, and star clusters. It assumes you are equipped with nothing more than a simple pair of binoculars, and that you know nothing of astronomy or the ...
... visible from the Southern Hemisphere, along with dozens of deep-sky sights of interest within each constellation, such as galaxies, binary stars, nebulae, and star clusters. It assumes you are equipped with nothing more than a simple pair of binoculars, and that you know nothing of astronomy or the ...
Magnetic fields in Local Group dwarf irregulars⋆
... Small Magellanic Cloud (SMC), a weak total field of about 3 μG was found, partly on large-scales (Mao et al. 2008). Since all these galaxies are optically bright and nearby objects, the detection of magnetic fields in them may be influenced by strong selection effects. The question then arises of whe ...
... Small Magellanic Cloud (SMC), a weak total field of about 3 μG was found, partly on large-scales (Mao et al. 2008). Since all these galaxies are optically bright and nearby objects, the detection of magnetic fields in them may be influenced by strong selection effects. The question then arises of whe ...
WILLIAM HERSCHEL AND THE `GARNET` STARS: μ CEPHEI AND
... Abstract: Although William Herschel‘s ‗Garnet Star‘ (µ Cephei) is a prominent object, the story of the discovery of this famous red star is not well documented. Prior to and after Herschel, the identification of this star was the subject of confusion in various catalogues and atlases. The case is co ...
... Abstract: Although William Herschel‘s ‗Garnet Star‘ (µ Cephei) is a prominent object, the story of the discovery of this famous red star is not well documented. Prior to and after Herschel, the identification of this star was the subject of confusion in various catalogues and atlases. The case is co ...
possibilities for the presence of dust in polars
... of Porb P 1 day. Due to its large specific orbital angular momentum, the mass lost from the secondary star does not fall directly onto the WD. In most CVs, it instead settles into a disk around the primary star before losing enough angular momentum through viscous processes to finally accrete onto t ...
... of Porb P 1 day. Due to its large specific orbital angular momentum, the mass lost from the secondary star does not fall directly onto the WD. In most CVs, it instead settles into a disk around the primary star before losing enough angular momentum through viscous processes to finally accrete onto t ...
Lu_Ye
... The tidal disruption of a solar type star by an IMBH with a mass of 2104Msoalr is proposed for the special event of GRB 060614, which is nearby long burst but is not associated with a supernova ...
... The tidal disruption of a solar type star by an IMBH with a mass of 2104Msoalr is proposed for the special event of GRB 060614, which is nearby long burst but is not associated with a supernova ...
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.