The 3-D shaping of NGC 6741: a massive, fast
... interference filter to isolate a single order. The same is valid for the reduction and investigation methods: so far long-slit echellograms have been used to obtain, either the kinematics in a few ions (in general, [O III], H I and [N II]), or the “average” nebular properties (physical conditions, i ...
... interference filter to isolate a single order. The same is valid for the reduction and investigation methods: so far long-slit echellograms have been used to obtain, either the kinematics in a few ions (in general, [O III], H I and [N II]), or the “average” nebular properties (physical conditions, i ...
The Swift satellite lives up to its name, revealing cosmic
... panying supernova component (expected for nearby long GRBs) found nothing to stringent limits, and together with the elliptical host galaxy this provided evidence in support of an origin for short bursts which is completely different from the massive star origins of their long-duration cousins: the ...
... panying supernova component (expected for nearby long GRBs) found nothing to stringent limits, and together with the elliptical host galaxy this provided evidence in support of an origin for short bursts which is completely different from the massive star origins of their long-duration cousins: the ...
A Study of the Nature and Representative Features of Supernova
... single stellar progenitor. No central core is left behind in the remnant. These supernovae are important because they can be used as “standard candles” for distance determination of their host galaxy. They all are believed to reach an absolute blue (B) magnitude of around +19.7 (Branch D. and Miller ...
... single stellar progenitor. No central core is left behind in the remnant. These supernovae are important because they can be used as “standard candles” for distance determination of their host galaxy. They all are believed to reach an absolute blue (B) magnitude of around +19.7 (Branch D. and Miller ...
First Results from the WISE Enhanced Resolution Galaxy Atlas
... in combination, reveal the internal life cycle of galaxies. The infrared window, for example, has dual capability: sensitive to stellar light from the evolved population of stars and relatively low-temperature processes from the interstellar medium and star formation regions. It is ideally suited fo ...
... in combination, reveal the internal life cycle of galaxies. The infrared window, for example, has dual capability: sensitive to stellar light from the evolved population of stars and relatively low-temperature processes from the interstellar medium and star formation regions. It is ideally suited fo ...
Massive Star Formation - Max-Planck
... Σ ∼ 100 M pc−2 (Solomon et al., 1987) (see Tan et al., 2013a for detailed discussion of the methods for estimating Σ for the objects plotted here), although denser examples have been found in Henize 2-10 (Santangelo et al., 2009). The 13 CO-defined clouds of RomanDuval et al. (2010) are indicated, ...
... Σ ∼ 100 M pc−2 (Solomon et al., 1987) (see Tan et al., 2013a for detailed discussion of the methods for estimating Σ for the objects plotted here), although denser examples have been found in Henize 2-10 (Santangelo et al., 2009). The 13 CO-defined clouds of RomanDuval et al. (2010) are indicated, ...
Spectral Matching for Elemental Abundances of Evolved Stars of Globular Clusters
... k-means clustering analysis was used to group the stars in ω Cen into four homogeneous groups based upon these abundances. These groups suggest that there were at least four main periods of star formation in the cluster. The exact order of these star formation events is not yet understood, with some ...
... k-means clustering analysis was used to group the stars in ω Cen into four homogeneous groups based upon these abundances. These groups suggest that there were at least four main periods of star formation in the cluster. The exact order of these star formation events is not yet understood, with some ...
The evolution of organic matter in space
... mass leading to carbon and heavier elements, and up to 56 Fe for the more massive stars. Heavier elements than iron are formed during the final stages of stars in stellar explosions by neutron absorption (s and r processes). In this phase, no equilibrium can be reached: the stars undergo mass loss ei ...
... mass leading to carbon and heavier elements, and up to 56 Fe for the more massive stars. Heavier elements than iron are formed during the final stages of stars in stellar explosions by neutron absorption (s and r processes). In this phase, no equilibrium can be reached: the stars undergo mass loss ei ...
Hot Gas In and Around Elliptical Galaxies William G. Mathews
... be possible in localized regions of high metallicity such as remnants of Type Ia explosions or if cold gas rapidly mixes with the hot gas. Cooling may also be very rapid in the dust-rich gas recently ejected from evolving stars. These processes have not been studied in detail. The currently most pop ...
... be possible in localized regions of high metallicity such as remnants of Type Ia explosions or if cold gas rapidly mixes with the hot gas. Cooling may also be very rapid in the dust-rich gas recently ejected from evolving stars. These processes have not been studied in detail. The currently most pop ...
Particle-Gas Dynamics and Primary Accretion
... rized in Boss and Goswami (2006) and Russell et al. (2006); see also the review by Calvet et al. (2000). The typical nebula mass M (98% hydrogen and helium) is a small fraction (0.02–0.2) of the stellar mass M*, and cannot yet be measured directly. Current estimates of the surface gas mass density σ ...
... rized in Boss and Goswami (2006) and Russell et al. (2006); see also the review by Calvet et al. (2000). The typical nebula mass M (98% hydrogen and helium) is a small fraction (0.02–0.2) of the stellar mass M*, and cannot yet be measured directly. Current estimates of the surface gas mass density σ ...
Injection mechanisms of short-lived radionuclides and their
... accretion of the angrite parent body is inconsistent with initial Solar System 60Fe estimates inferred from Bishunpur and Semarkona chondrules, suggesting decoupling in the presence of 26Al and 60Fe in some early formed planetesimals. This could reflect heterogeneous distribution of 60Fe in the proto ...
... accretion of the angrite parent body is inconsistent with initial Solar System 60Fe estimates inferred from Bishunpur and Semarkona chondrules, suggesting decoupling in the presence of 26Al and 60Fe in some early formed planetesimals. This could reflect heterogeneous distribution of 60Fe in the proto ...
Anisotropy of the Hectometer Cosmic Radio Background
... direction toward the Galactic source was close to 90°, and its increase in the April 5, 1998 and October 4, 1998 sessions, when the source was virtually on this line (see Fig. 3), can also be explained in terms of the model of two sources. The resulting modulation index and ecliptic longitude of the ...
... direction toward the Galactic source was close to 90°, and its increase in the April 5, 1998 and October 4, 1998 sessions, when the source was virtually on this line (see Fig. 3), can also be explained in terms of the model of two sources. The resulting modulation index and ecliptic longitude of the ...
Small star patterns for telescopes and binoculars Demelza Ramakers
... size of the object. Because most asterisms are more familiar with their nicknames, I use these where possible in the description. The number in front of the name stands for the asterism number in which I numbered them. Finally follows the description. As I mentioned before, I haven’t seen all asteri ...
... size of the object. Because most asterisms are more familiar with their nicknames, I use these where possible in the description. The number in front of the name stands for the asterism number in which I numbered them. Finally follows the description. As I mentioned before, I haven’t seen all asteri ...
CHARACTERIZING DUST ATTENUATION IN LOCAL STAR FORMING GALAXIES: UV AND... REDDENING ABSTRACT The dust attenuation for a sample of ∼10000 local (z ....
... with short-lived dense clouds where massive stars form HII regions and another associated with the diffuse interstellar medium. For this study, we follow the methodology used in Calzetti et al. (1994) to determine the behavior of dust attenuation in a large sample of SFGs with a wide range of proper ...
... with short-lived dense clouds where massive stars form HII regions and another associated with the diffuse interstellar medium. For this study, we follow the methodology used in Calzetti et al. (1994) to determine the behavior of dust attenuation in a large sample of SFGs with a wide range of proper ...
The physics of star formation
... Star formation occurs as a result of the action of gravity on a wide range of scales, and different mechanisms may be important on different scales, depending on the forces opposing gravity. On galactic scales, the tendency of interstellar matter to condense under gravity into star-forming clouds is ...
... Star formation occurs as a result of the action of gravity on a wide range of scales, and different mechanisms may be important on different scales, depending on the forces opposing gravity. On galactic scales, the tendency of interstellar matter to condense under gravity into star-forming clouds is ...
High precision effective temperatures for 181 F-
... between A0 and K3 by using IRFM and achieved an accuracy of 0.9%. DB98 derived Teff for 537 dwarfs and giants by the empirical method of surface brightness and Johnson broadband (V − K) color, the accuracy claimed is ±1%. Whenever 2 or 3 estimates were available for a given star, we averaged them wi ...
... between A0 and K3 by using IRFM and achieved an accuracy of 0.9%. DB98 derived Teff for 537 dwarfs and giants by the empirical method of surface brightness and Johnson broadband (V − K) color, the accuracy claimed is ±1%. Whenever 2 or 3 estimates were available for a given star, we averaged them wi ...
Astrochemistry of dense protostellar and protoplanetary environments
... physical evolution in its diversity requires a combination of observations from infrared (IR) to millimeter (mm) wavelengths, where gaseous and solid material have their principal spectroscopic features and where the extinction is small enough to penetrate the dusty regions. The different evolutiona ...
... physical evolution in its diversity requires a combination of observations from infrared (IR) to millimeter (mm) wavelengths, where gaseous and solid material have their principal spectroscopic features and where the extinction is small enough to penetrate the dusty regions. The different evolutiona ...
The physics and modes of star cluster formation: observations
... Downloaded from http://rsta.royalsocietypublishing.org/ on June 17, 2017 ...
... Downloaded from http://rsta.royalsocietypublishing.org/ on June 17, 2017 ...
The physics of star formation
... Stars are the fundamental units of luminous matter in the universe, and they are responsible, directly or indirectly, for most of what we see when we observe it. They also serve as our primary tracers of the structure and evolution of the universe and its contents. Consequently, it is of central imp ...
... Stars are the fundamental units of luminous matter in the universe, and they are responsible, directly or indirectly, for most of what we see when we observe it. They also serve as our primary tracers of the structure and evolution of the universe and its contents. Consequently, it is of central imp ...
Chapter 12
... your hand motionless at arm’s length and shift your head from side to side. Your hand seems to move against the background even though in reality it is your head that has changed position, not your hand. This simple demonstration illustrates how parallax gives a clue to an object’s distance. If you ...
... your hand motionless at arm’s length and shift your head from side to side. Your hand seems to move against the background even though in reality it is your head that has changed position, not your hand. This simple demonstration illustrates how parallax gives a clue to an object’s distance. If you ...
The physics of star formation - Yale Astronomy
... Stars are the fundamental units of luminous matter in the universe, and they are responsible, directly or indirectly, for most of what we see when we observe it. They also serve as our primary tracers of the structure and evolution of the universe and its contents. Consequently, it is of central imp ...
... Stars are the fundamental units of luminous matter in the universe, and they are responsible, directly or indirectly, for most of what we see when we observe it. They also serve as our primary tracers of the structure and evolution of the universe and its contents. Consequently, it is of central imp ...
An Expanded View of the Universe
... the Universe? Black holes have puzzled physicists and astronomers since they were first postulated in relativistic form a century ago by Karl Schwarzschild. Observations have demonstrated that these bizarre objects really exist. And on a grand scale, too: not only have black holes been found with ma ...
... the Universe? Black holes have puzzled physicists and astronomers since they were first postulated in relativistic form a century ago by Karl Schwarzschild. Observations have demonstrated that these bizarre objects really exist. And on a grand scale, too: not only have black holes been found with ma ...
spatially resolved star formation history of milky way satellites
... satellites there is another galaxy similar in size than the Milky Way, called Andromeda or Messier 31 (M31), which, as the Milky Way, has its own satellites. These two big galaxies and their own satellites form a self-gravitating association called the Local Group, and hence, the satellite galaxies ...
... satellites there is another galaxy similar in size than the Milky Way, called Andromeda or Messier 31 (M31), which, as the Milky Way, has its own satellites. These two big galaxies and their own satellites form a self-gravitating association called the Local Group, and hence, the satellite galaxies ...
... In the RRL data base of GEOS (2012) one can find a list of 96 times of maxima and the corresponding O-C diagram built with the ephemerides 2419130.305+0.28779276 E is reproduced in Figure 4. Visual observations show a particularly large scatter at HJD ∼ 2443800 which may be due to their larger uncer ...
The Sky This Month
... • The middle “star” / “fuzzy thing” in Orion’s sword : Mag 4.0. • Bright diffuse nebula with brightest central region about 1° across. • 100 ly away and ~60 ly across. • The closest known star forming region – filled with lots of young stars (Trapezium cluster). • Galileo discovered the Trapezium cl ...
... • The middle “star” / “fuzzy thing” in Orion’s sword : Mag 4.0. • Bright diffuse nebula with brightest central region about 1° across. • 100 ly away and ~60 ly across. • The closest known star forming region – filled with lots of young stars (Trapezium cluster). • Galileo discovered the Trapezium cl ...
Properties of Galactic early-type O
... Aims. We aim to constrain the properties and evolutionary status of early and mid-spectral type supergiants (from O4 to O7.5). These posses the highest mass-loss rates among the O stars, and exhibit conspicuous wind profiles. Methods. Using the non-LTE wind code cmfgen we simultaneously analyzed the ...
... Aims. We aim to constrain the properties and evolutionary status of early and mid-spectral type supergiants (from O4 to O7.5). These posses the highest mass-loss rates among the O stars, and exhibit conspicuous wind profiles. Methods. Using the non-LTE wind code cmfgen we simultaneously analyzed the ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.