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... A disc-like structure with a center 100-150 pc from the Sun Inclined respect to the galactic plane by ~20o 2/3 of massive stars in 600 pc from the Sun belong to the Belt ...
... A disc-like structure with a center 100-150 pc from the Sun Inclined respect to the galactic plane by ~20o 2/3 of massive stars in 600 pc from the Sun belong to the Belt ...
Chromospherically young, kinematically old stars
... see also Jeffries & Jewell 1993), who studied the kinematics of active and inactive stars. The active stars are concentrated in a region of low velocities in a space velocity diagram, as expected for young objects; on the other hand, the inactive stars are scattered in this diagram, just like old st ...
... see also Jeffries & Jewell 1993), who studied the kinematics of active and inactive stars. The active stars are concentrated in a region of low velocities in a space velocity diagram, as expected for young objects; on the other hand, the inactive stars are scattered in this diagram, just like old st ...
Finnish Centre for Astronomy with ESO
... The year 2014 marked the 5th year of operation for FINCA, administratively a Special Unit of the University of Turku, and funded by the Ministry of Education and Culture, and by the participating universities (Aalto, Helsinki, Oulu and Turku). The highest decision-making body is the Board, chaired b ...
... The year 2014 marked the 5th year of operation for FINCA, administratively a Special Unit of the University of Turku, and funded by the Ministry of Education and Culture, and by the participating universities (Aalto, Helsinki, Oulu and Turku). The highest decision-making body is the Board, chaired b ...
2 The Concept of “Spectral Classes”
... Assignment of Spectral Peculiarities, P1P2P3P4 All stars including the standards are peculiar at some level. Hence, the most complicated part of any classification system is the array of spectral peculiarities, usually designated by a single letter or character. The descriptions of these attributes ...
... Assignment of Spectral Peculiarities, P1P2P3P4 All stars including the standards are peculiar at some level. Hence, the most complicated part of any classification system is the array of spectral peculiarities, usually designated by a single letter or character. The descriptions of these attributes ...
4-H MOTTO
... Light is one of the most important aspects of astronomy. Everything that we can see in the night sky, whether it is a star, a planet or a galaxy, emits light. If an object did not emit light then we would not know it was there. Objects such as stars, galaxies and nebulae generate their own light whe ...
... Light is one of the most important aspects of astronomy. Everything that we can see in the night sky, whether it is a star, a planet or a galaxy, emits light. If an object did not emit light then we would not know it was there. Objects such as stars, galaxies and nebulae generate their own light whe ...
The self-enrichment of galactic halo globular clusters: a clue to their
... interstellar medium of the nearby dwarf galaxy IC2574, Walter et al. (1998) have studied a supergiant HI shell obviously produced by the combined effects of stellar winds and supernova explosions. A major star formation event (equivalent to our first generation) has likely taken place at the center ...
... interstellar medium of the nearby dwarf galaxy IC2574, Walter et al. (1998) have studied a supergiant HI shell obviously produced by the combined effects of stellar winds and supernova explosions. A major star formation event (equivalent to our first generation) has likely taken place at the center ...
Chemical abundances and winds of massive stars in M31: a Btype
... (1987), although little quantitative analysis has been carried out to date. The only detailed studies of Wolf – Rayet stars beyond the Magellanic Clouds have been studies of late WN stars in M33 by Smith et al. (1995) and Crowther et al. (1997). Bianchi et al. (1996b) have published UV spectroscopy ...
... (1987), although little quantitative analysis has been carried out to date. The only detailed studies of Wolf – Rayet stars beyond the Magellanic Clouds have been studies of late WN stars in M33 by Smith et al. (1995) and Crowther et al. (1997). Bianchi et al. (1996b) have published UV spectroscopy ...
Chemical abundances and winds of massive stars in M31: a B
... (WLR, e.g. Kudritzki et al. 1999). An investigation of the stellar wind properties of O-, B- and A-supergiants in Local Group galaxies with well defined distances will, therefore, allow us to test the concept of the WLR and its applicability for distance determinations. Numerous surveys have identif ...
... (WLR, e.g. Kudritzki et al. 1999). An investigation of the stellar wind properties of O-, B- and A-supergiants in Local Group galaxies with well defined distances will, therefore, allow us to test the concept of the WLR and its applicability for distance determinations. Numerous surveys have identif ...
Lecture 8: Spiral Structure
... Suppose cars traveling on a long highway at a speed exceeding the speed limit. Also traveling a long the road, at less than the speed limit, is a police car (car x) with its radar on. Observing from a helicopter high in the sky, we see the cars fairly evenly distributed along the highway except aro ...
... Suppose cars traveling on a long highway at a speed exceeding the speed limit. Also traveling a long the road, at less than the speed limit, is a police car (car x) with its radar on. Observing from a helicopter high in the sky, we see the cars fairly evenly distributed along the highway except aro ...
Penn State Astronomy 11 Laboratory
... Mizar and Alcor in Ursa Major (double star) Albireo in Cygnus (double star) M13 in Hercules (a globular cluster) The Andromeda Galaxy (M31) ...
... Mizar and Alcor in Ursa Major (double star) Albireo in Cygnus (double star) M13 in Hercules (a globular cluster) The Andromeda Galaxy (M31) ...
Dust and molecular gas in the most distant quasars
... • It is likely that active star formation is ongoing in the host galaxies of the strong millimeter detected quasars at z~6. – Star formation rate: ≥103 Msun yr-1. – Star formation efficiency: comparable to ULIRGs and SMGs. • Gas mass: ~1010 Msun, which will turn to stars via the massive starburst. • ...
... • It is likely that active star formation is ongoing in the host galaxies of the strong millimeter detected quasars at z~6. – Star formation rate: ≥103 Msun yr-1. – Star formation efficiency: comparable to ULIRGs and SMGs. • Gas mass: ~1010 Msun, which will turn to stars via the massive starburst. • ...
Riccioli Measures the Stars: Observations of the
... the stars dwarf the orbit of the Earth.* Riccioli also critiques Landsbergius who cites naked eye measurements of star sizes, including those of Tycho Brahe, that put the observed diameter of first magnitude stars at a minute (60‟‟) or greater, but who then adds that through the telescope star diam ...
... the stars dwarf the orbit of the Earth.* Riccioli also critiques Landsbergius who cites naked eye measurements of star sizes, including those of Tycho Brahe, that put the observed diameter of first magnitude stars at a minute (60‟‟) or greater, but who then adds that through the telescope star diam ...
Supernovae - University of Texas Astronomy Home Page
... observe a young expanding gaseous remnant of an exploded star, a powerful emitter of radio radiation known as Cassiopeia A. From the present size and rate of expansion of the remnant, we deduce that the explosion that gave rise to Cas A occurred in about 1667. By rights, this should have been Newton ...
... observe a young expanding gaseous remnant of an exploded star, a powerful emitter of radio radiation known as Cassiopeia A. From the present size and rate of expansion of the remnant, we deduce that the explosion that gave rise to Cas A occurred in about 1667. By rights, this should have been Newton ...
1 Astrobiologically Interesting Stars within 10
... initially, in the outer limits of the stellar CHZ. Previous efforts, mainly targeted at selecting nearby stars in terms of their suitability to SETI programs, have not included the full set of criteria presented here (e.g., Blair et al., 1992, Henry et al., 1995), and have generally applied them wit ...
... initially, in the outer limits of the stellar CHZ. Previous efforts, mainly targeted at selecting nearby stars in terms of their suitability to SETI programs, have not included the full set of criteria presented here (e.g., Blair et al., 1992, Henry et al., 1995), and have generally applied them wit ...
FREE Sample Here
... 26. Assume the size of the Sun is represented by a baseball with the Earth is about 15 meters (150 million km or 8 light minutes) away. How far away, to scale, would the nearest stars to the Sun be? Pick the closest answer. a. About the distance between New York and Boston. (330 km) b. 100 meters aw ...
... 26. Assume the size of the Sun is represented by a baseball with the Earth is about 15 meters (150 million km or 8 light minutes) away. How far away, to scale, would the nearest stars to the Sun be? Pick the closest answer. a. About the distance between New York and Boston. (330 km) b. 100 meters aw ...
Using color photometry to separate transiting exoplanets from false
... binary eclipses, this technique cannot reliably identify blends, a chance overlap of a faint background eclipsing binary with an ordinary foreground star. Blends generally have no observable radial velocity shifts, as the foreground star is brighter by several magnitudes and therefore dominates the ...
... binary eclipses, this technique cannot reliably identify blends, a chance overlap of a faint background eclipsing binary with an ordinary foreground star. Blends generally have no observable radial velocity shifts, as the foreground star is brighter by several magnitudes and therefore dominates the ...
The physics and modes of star cluster formation: observations
... is considerably more difficult, especially for intrinsically faint members whose numbers are only comparable to or significantly lower than those of the background/foreground stellar field population. The size of the cluster’s membership can be determined statistically through comparison with the backg ...
... is considerably more difficult, especially for intrinsically faint members whose numbers are only comparable to or significantly lower than those of the background/foreground stellar field population. The size of the cluster’s membership can be determined statistically through comparison with the backg ...
flare swg usa
... Fitting SEDS: The long-λ fluxes from cool dust have ambiguous SED fits, while higher spatial resolution, near-IR fluxes from clustered sources are often very much fainter. FLARE can reach ~8 mag deeper than IRAC surveys at 3.5 μm, enabling the measurement of the NIR SEDs of young (<104 yr old) ...
... Fitting SEDS: The long-λ fluxes from cool dust have ambiguous SED fits, while higher spatial resolution, near-IR fluxes from clustered sources are often very much fainter. FLARE can reach ~8 mag deeper than IRAC surveys at 3.5 μm, enabling the measurement of the NIR SEDs of young (<104 yr old) ...
Star formation in a galactic outflow
... the ratio between ionizing photon flux and gas density; when divided by the speed of light it is the adimensional ionization parameter U) much lower than typically observed in star-forming galaxies. Yet, despite the gas density in the outflow (~600-1,500 cm-3, as inferred from the [SII] doublet) bei ...
... the ratio between ionizing photon flux and gas density; when divided by the speed of light it is the adimensional ionization parameter U) much lower than typically observed in star-forming galaxies. Yet, despite the gas density in the outflow (~600-1,500 cm-3, as inferred from the [SII] doublet) bei ...
Interpretation of the Helix Planetary Nebula using Hydro
... WD growth of slowly dying ≤ M size stars fed by JPP comets is slower than the standard model SNe Ia events (see §2.3.1) where superwinds dump most of the mass of relatively short-lived 3 − 9M intermediate size stars into the ISM. Few SNe Ia events are seen at large redshifts, and this may be why. ...
... WD growth of slowly dying ≤ M size stars fed by JPP comets is slower than the standard model SNe Ia events (see §2.3.1) where superwinds dump most of the mass of relatively short-lived 3 − 9M intermediate size stars into the ISM. Few SNe Ia events are seen at large redshifts, and this may be why. ...
Brightness and Flux Density
... emission from our Galaxy). In practice, when do we use spectral brightness and when do we use flux density to describe a source? If a source is unresolved, meaning that it is much smaller in angular size than the point-source response of the eye or telescope observing it, its flux density can be mea ...
... emission from our Galaxy). In practice, when do we use spectral brightness and when do we use flux density to describe a source? If a source is unresolved, meaning that it is much smaller in angular size than the point-source response of the eye or telescope observing it, its flux density can be mea ...
Test 3 Review Clicker Questions
... a) there are no stars there. b) stars in that direction are obscured by interstellar gas. c) stars in that direction are obscured by interstellar dust. d) numerous black holes capture all the starlight behind them. ...
... a) there are no stars there. b) stars in that direction are obscured by interstellar gas. c) stars in that direction are obscured by interstellar dust. d) numerous black holes capture all the starlight behind them. ...
Perseus (constellation)
Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.