PPT presentation
... high L’s interpreted as due to sharp cutoff to upper mass limit of PN central stars. ...
... high L’s interpreted as due to sharp cutoff to upper mass limit of PN central stars. ...
our knowledge of high-mass star formation at the dawn of - CEA-Irfu
... massive cold molecular cores, or even infrared-dark clouds. In the subsequent phase, they have been named massive protostars, high-mass protostellar objects, or hot molecular cores. The better-known final phase would correspond to H ii regions being from hyper-compact to classical. Unfortunately, th ...
... massive cold molecular cores, or even infrared-dark clouds. In the subsequent phase, they have been named massive protostars, high-mass protostellar objects, or hot molecular cores. The better-known final phase would correspond to H ii regions being from hyper-compact to classical. Unfortunately, th ...
PPT presentation
... Contamination of the PN samples The contamination increases with distance to the galaxy. It is negligible for distances < 10 Mpc, as we just saw. At the distance of the Virgo cluster the luminosity function of the contaminants imitates the PNLF of a low-surfacedensity PN population at that distance ...
... Contamination of the PN samples The contamination increases with distance to the galaxy. It is negligible for distances < 10 Mpc, as we just saw. At the distance of the Virgo cluster the luminosity function of the contaminants imitates the PNLF of a low-surfacedensity PN population at that distance ...
Cassiopeia Kelly Pearce
... (Stars.Astro.Illinois.edu, Segin, 2010). It forms the outer most left point of the W and is the fifth brightest of all 5 stars. It is noticeably dimmer than the remaining stars but definitively forms the one of the outermost points of the shape. The next star to the right is Delta Cassiopeiae and is ...
... (Stars.Astro.Illinois.edu, Segin, 2010). It forms the outer most left point of the W and is the fifth brightest of all 5 stars. It is noticeably dimmer than the remaining stars but definitively forms the one of the outermost points of the shape. The next star to the right is Delta Cassiopeiae and is ...
1 Globular Cluster Systems - McMaster Physics and Astronomy
... and thus to elongate their whole distribution along the line of sight (roughly, the X axis). (3) The fundamental distance scale used by Shapley { essentially, the luminosity of the RR Lyraes or the tip of the red-giant branch { was about one magnitude brighter than the value adopted today; again, th ...
... and thus to elongate their whole distribution along the line of sight (roughly, the X axis). (3) The fundamental distance scale used by Shapley { essentially, the luminosity of the RR Lyraes or the tip of the red-giant branch { was about one magnitude brighter than the value adopted today; again, th ...
ATLAS lifts the Cup: discovery of a new Milky Way satellite in Crater⋆†
... population implies that star formation occurred in Crater perhaps as recently as 400 Myr ago. No globular cluster has ever accomplished the feat of prolonging its star formation by several Gyr. Therefore, if our hypothesis that the blue bright stars in Crater are blue loop giants is correct, the new ...
... population implies that star formation occurred in Crater perhaps as recently as 400 Myr ago. No globular cluster has ever accomplished the feat of prolonging its star formation by several Gyr. Therefore, if our hypothesis that the blue bright stars in Crater are blue loop giants is correct, the new ...
OBSERVATIONS OF PHYSICAL PROCESSES IN
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
A Spectroscopically Confirmed Excess of 24 micron Sources in a
... understanding the interplay between galaxy evolution and environment is to study galaxy groups because: 1) most galaxies in the local universe are in groups (e.g. Geller & Huchra 1983); and 2) hierarchical structure formation predicts that galaxy clusters assemble from the merger and accretion of sm ...
... understanding the interplay between galaxy evolution and environment is to study galaxy groups because: 1) most galaxies in the local universe are in groups (e.g. Geller & Huchra 1983); and 2) hierarchical structure formation predicts that galaxy clusters assemble from the merger and accretion of sm ...
Course Outline - Tony Bacigalupo
... The region of a galaxy beyond the visible halo where dark matter is believed to reside Composition? ...
... The region of a galaxy beyond the visible halo where dark matter is believed to reside Composition? ...
Collisions and Encounters of Stellar Systems
... A characteristic feature of collisions of stellar systems is the systematic transfer of energy from their relative orbital motion into random motions of their constituent particles. This process is simplest to understand in the limiting case of minor mergers, in which one system is much smaller than ...
... A characteristic feature of collisions of stellar systems is the systematic transfer of energy from their relative orbital motion into random motions of their constituent particles. This process is simplest to understand in the limiting case of minor mergers, in which one system is much smaller than ...
Hipparcos distance estimates of the Ophiuchus and the Lupus cloud
... dark molecular clouds and their dense cores. One of the main motivations for these investigations is the study of the process of star and planet formation in its entirety, and a deeper understanding of the effects of the local environment. A key aspect of the scientific analysis of a dark molecular c ...
... dark molecular clouds and their dense cores. One of the main motivations for these investigations is the study of the process of star and planet formation in its entirety, and a deeper understanding of the effects of the local environment. A key aspect of the scientific analysis of a dark molecular c ...
The 2008 RBSE Journal - National Optical Astronomy Observatory
... and usually end up being bigger than the originating galaxy. The smallest known are only a few tens of parsecs across, while the largest are known to be up to several megaparsecs. The average radio galaxy is usually typically hundreds of kiloparsecs across. This is about twice the size of the Milky ...
... and usually end up being bigger than the originating galaxy. The smallest known are only a few tens of parsecs across, while the largest are known to be up to several megaparsecs. The average radio galaxy is usually typically hundreds of kiloparsecs across. This is about twice the size of the Milky ...
The Birth Environment of the Solar System
... After extrapolating the data to include the full range of periods, the fraction of systems with giant planets is estimated to be about 20 percent (although larger fractions, perhaps up to 50 percent, remain possible). At this time, detection of planets with masses comparable to Earth is just out of ...
... After extrapolating the data to include the full range of periods, the fraction of systems with giant planets is estimated to be about 20 percent (although larger fractions, perhaps up to 50 percent, remain possible). At this time, detection of planets with masses comparable to Earth is just out of ...
Colour-magnitude diagrams of the post
... can be considered a member. Goranskii determined a period of 0.5752 days, so that the cluster can be tentatively classified as Oosterhoff type I. 5. Conclusions Cluster parameters based on CCD photometry were derived for NGC 6256 and NGC 6717. They are both located in the bulge, but are not metal-ri ...
... can be considered a member. Goranskii determined a period of 0.5752 days, so that the cluster can be tentatively classified as Oosterhoff type I. 5. Conclusions Cluster parameters based on CCD photometry were derived for NGC 6256 and NGC 6717. They are both located in the bulge, but are not metal-ri ...
ASPEN WORKSHOP 2003
... WARNING: These notes were not reviewed by the speakers. For more reliable summaries of what they said (without my editorializing), you should ask the individual speakers for their Powerpoint presentations. Also, notes for several talks are missing since I did not have a working laptop for them and h ...
... WARNING: These notes were not reviewed by the speakers. For more reliable summaries of what they said (without my editorializing), you should ask the individual speakers for their Powerpoint presentations. Also, notes for several talks are missing since I did not have a working laptop for them and h ...
Lecture 2 Astronomical Distances
... HST sees Cepheids to D = 10-20 Mpc. H0 x D = 70 x 15 ~ 1000 km/s. not really far enough galaxy pecular velocities ~500 km/s. galaxies falling toward Virgo cluster. ...
... HST sees Cepheids to D = 10-20 Mpc. H0 x D = 70 x 15 ~ 1000 km/s. not really far enough galaxy pecular velocities ~500 km/s. galaxies falling toward Virgo cluster. ...
21 -26 August University of Exeter
... Investigating the dynamics of the interstellar medium (ISM) is key to gaining insight into the formation of starforming filaments in molecular clouds (MCs). A plethora of numerical and analytical models associate the origin of this filamentary structure to the interplay between self-gravity and magn ...
... Investigating the dynamics of the interstellar medium (ISM) is key to gaining insight into the formation of starforming filaments in molecular clouds (MCs). A plethora of numerical and analytical models associate the origin of this filamentary structure to the interplay between self-gravity and magn ...
Sample pages 1 PDF
... and the Orion Nebula is no exception. Long-exposure photographs reveal all sorts of complex features, including star clusters, reflection nebulae, and clouds of gas and dust. The Hubble Telescope has also shown evidence of protoplanetary discs, known as proplyds, meaning that at least some of the yo ...
... and the Orion Nebula is no exception. Long-exposure photographs reveal all sorts of complex features, including star clusters, reflection nebulae, and clouds of gas and dust. The Hubble Telescope has also shown evidence of protoplanetary discs, known as proplyds, meaning that at least some of the yo ...
The Gould Belt
... Pöppel has pointed out [26] that only the relatively near stars no later than spectral class B2.5 can be said reliably to belong to the Gould belt. There are, however, very few of them. In order to assign stars from other spectral classes to the belt, various methods of distinguishing the stars fro ...
... Pöppel has pointed out [26] that only the relatively near stars no later than spectral class B2.5 can be said reliably to belong to the Gould belt. There are, however, very few of them. In order to assign stars from other spectral classes to the belt, various methods of distinguishing the stars fro ...
POSTERS SESSION I: Atmospheres of Massive Stars
... wind, probably triggered by a companion star’s periastron approach. This indicates a surface instability that was not predicted and is stronger than one would normally have expected based on tidal and radiative effects. The hypothetical companion object continuously alters the primary star’s surface ...
... wind, probably triggered by a companion star’s periastron approach. This indicates a surface instability that was not predicted and is stronger than one would normally have expected based on tidal and radiative effects. The hypothetical companion object continuously alters the primary star’s surface ...
Bonnell_2015_MNRAS_Early - St Andrews Research Repository
... a rate substantially slower than the freefall rate in the dense gas. This decoupling is due to the weakening of, and expulsion of gas from, the deepest parts of the clouds’ potential wells where most of the star formation occurs in the control simulations. This results in large fractions of the stel ...
... a rate substantially slower than the freefall rate in the dense gas. This decoupling is due to the weakening of, and expulsion of gas from, the deepest parts of the clouds’ potential wells where most of the star formation occurs in the control simulations. This results in large fractions of the stel ...
Abundances and possible diffusion of elements in M 67 stars⋆
... effects, albeit of smaller overall amplitude, have recently been traced in NGC 6752 at somewhat higher metallicities (Gruyters et al. 2013). In M 4, at roughly one tenth solar metallicity, no abundance trend in iron was found between the turn-off point and the red giants (Mucciarelli et al. 2011), pos ...
... effects, albeit of smaller overall amplitude, have recently been traced in NGC 6752 at somewhat higher metallicities (Gruyters et al. 2013). In M 4, at roughly one tenth solar metallicity, no abundance trend in iron was found between the turn-off point and the red giants (Mucciarelli et al. 2011), pos ...
The Formation and Evolution of the Milky Way
... 2). The spiral disk itself can be subdivided into a thin disk, which rises about 1,000 light-years above and below the galactic mid-plane, and a thick disk, which extends to about 3,500 light-years on either side of the plane. The relative flatness of our galaxy is evident when one considers that th ...
... 2). The spiral disk itself can be subdivided into a thin disk, which rises about 1,000 light-years above and below the galactic mid-plane, and a thick disk, which extends to about 3,500 light-years on either side of the plane. The relative flatness of our galaxy is evident when one considers that th ...
the stebbins galaxy: the origins of interstellar medium studies
... the inclination of many astronomers to understand the spiral nebulae as vast stellar structures (‗island universes‘ as they said) and perhaps even galaxies comparable to our own. Moreover, between about 1928 and 1930, the work of Bertil Lindblad (1895 –1965), Jan Oort (1900 –1992), and John Plaskett ...
... the inclination of many astronomers to understand the spiral nebulae as vast stellar structures (‗island universes‘ as they said) and perhaps even galaxies comparable to our own. Moreover, between about 1928 and 1930, the work of Bertil Lindblad (1895 –1965), Jan Oort (1900 –1992), and John Plaskett ...
Open cluster
An open cluster, also known as galactic cluster, is a group of up to a few thousand stars that were formed from the same giant molecular cloud and have roughly the same age. More than 1,100 open clusters have been discovered within the Milky Way Galaxy, and many more are thought to exist. They are loosely bound by mutual gravitational attraction and become disrupted by close encounters with other clusters and clouds of gas as they orbit the galactic center, resulting in a migration to the main body of the galaxy as well as a loss of cluster members through internal close encounters. Open clusters generally survive for a few hundred million years, with the most massive ones surviving for a few billion years. In contrast, the more massive globular clusters of stars exert a stronger gravitational attraction on their members, and can survive for longer. Open clusters have been found only in spiral and irregular galaxies, in which active star formation is occurring.Young open clusters may still be contained within the molecular cloud from which they formed, illuminating it to create an H II region. Over time, radiation pressure from the cluster will disperse the molecular cloud. Typically, about 10% of the mass of a gas cloud will coalesce into stars before radiation pressure drives the rest of the gas away.Open clusters are key objects in the study of stellar evolution. Because the cluster members are of similar age and chemical composition, their properties (such as distance, age, metallicity and extinction) are more easily determined than they are for isolated stars. A number of open clusters, such as the Pleiades, Hyades or the Alpha Persei Cluster are visible with the naked eye. Some others, such as the Double Cluster, are barely perceptible without instruments, while many more can be seen using binoculars or telescopes. The Wild Duck Cluster, M11, is an example.