here
... Bending and stretching vibrations of hydrocarbon bonds • Comparison with laboratory IR spectra • But conditions very different (ionized, isolated) ...
... Bending and stretching vibrations of hydrocarbon bonds • Comparison with laboratory IR spectra • But conditions very different (ionized, isolated) ...
Diapositiva 1 - Dipartimento di Fisica
... The first extrasolar planet around a main-sequence star was found in 1995 around 51 Pegasi, a G5V star, analyzing the radial velocity variations of the parent star due to its motion around the barycenter of the system [3]. The radial velocity method allow to detect only Jupiter-like planets, in part ...
... The first extrasolar planet around a main-sequence star was found in 1995 around 51 Pegasi, a G5V star, analyzing the radial velocity variations of the parent star due to its motion around the barycenter of the system [3]. The radial velocity method allow to detect only Jupiter-like planets, in part ...
Metal Abundances of Subdwarf B Stars from SPY
... which cannot be explained in the framework of diffusion alone. Nuclear processed material must have been transported to the surface. The late hot-flasher scenario may provide a possible explanation for this effect. ...
... which cannot be explained in the framework of diffusion alone. Nuclear processed material must have been transported to the surface. The late hot-flasher scenario may provide a possible explanation for this effect. ...
August - Naples Free-Net
... through a telescope with your own eyes, unless that telescope was many feet in diameter, you’ve probably never seen a galaxy’s spiral structure for yourself. In fact, the very closest large galaxy to usAndromeda, M31wasn’t discovered to be a spiral until 1888, despite being clearly visible to the ...
... through a telescope with your own eyes, unless that telescope was many feet in diameter, you’ve probably never seen a galaxy’s spiral structure for yourself. In fact, the very closest large galaxy to usAndromeda, M31wasn’t discovered to be a spiral until 1888, despite being clearly visible to the ...
a cluster of stars - PEO - Wisconsin State Chapter
... distinguish several of the constellations—the Big Dipper, the Southern Cross; now, the dark sky reveals its most spectacular sight, for it is filled almost to overflowing with hundreds, even thousands and millions, of stars like so many flickering fire-flies, glowing candles, or sparkling diamonds. ...
... distinguish several of the constellations—the Big Dipper, the Southern Cross; now, the dark sky reveals its most spectacular sight, for it is filled almost to overflowing with hundreds, even thousands and millions, of stars like so many flickering fire-flies, glowing candles, or sparkling diamonds. ...
–1– 1. Stellar Evolution For Massive Stars 1.1. The Importance of
... during the main sequence phase is proportional to ∆M/M ∝ M 1.8 . Because of this strong dependence on mass, mass loss becomes very important for high mass stars. If high mass 0Z stars really do have very weak winds, they will not be very effective at polluting the ISM with nuclear processed material ...
... during the main sequence phase is proportional to ∆M/M ∝ M 1.8 . Because of this strong dependence on mass, mass loss becomes very important for high mass stars. If high mass 0Z stars really do have very weak winds, they will not be very effective at polluting the ISM with nuclear processed material ...
Slide 1
... role in the type of period evolution. The correlation between these changes and thermal pulses is not so obvious: among the stars studied by Lebzelter and Hron (2003), SW Gem and TW Peg do not present Technetium; the other stars have not been studied. Moreover the presence of close modes of pulsatio ...
... role in the type of period evolution. The correlation between these changes and thermal pulses is not so obvious: among the stars studied by Lebzelter and Hron (2003), SW Gem and TW Peg do not present Technetium; the other stars have not been studied. Moreover the presence of close modes of pulsatio ...
THE MYSTERIOUS SICKLE OBJECT IN THE CARINA NEBULA: A
... a bow shock associated with the B1.5 V star Trumpler 14 MJ 218 (MJ 218 hereafter) listed in Massey & Johnson (1993). We discuss a possible link between the star, the Sickle and the clump and argue that the star is moving supersonically through the ambient density gradient on the front side of the ob ...
... a bow shock associated with the B1.5 V star Trumpler 14 MJ 218 (MJ 218 hereafter) listed in Massey & Johnson (1993). We discuss a possible link between the star, the Sickle and the clump and argue that the star is moving supersonically through the ambient density gradient on the front side of the ob ...
Characterizing the Cool KOIs
... • The Kepler-32 planets are representative of all of Keplerʼs M dwarf planets, and therefore M dwarfs throughout the Galaxy " • These are powerful constraints on the timescale and nature of the mechanisms that form some of the most numerous planetary systems in the Galaxy!" • The Solar System is ...
... • The Kepler-32 planets are representative of all of Keplerʼs M dwarf planets, and therefore M dwarfs throughout the Galaxy " • These are powerful constraints on the timescale and nature of the mechanisms that form some of the most numerous planetary systems in the Galaxy!" • The Solar System is ...
The Sun The Sun is a very typical main sequence star. It contains 1000
... diffusion. Here, the high energy photons generated by nuclear reac9ons are sca_ered, absorbed and re-‐emi_ed by the atoms and free electrons, which causes them to degrade in energy. The fact that heat i ...
... diffusion. Here, the high energy photons generated by nuclear reac9ons are sca_ered, absorbed and re-‐emi_ed by the atoms and free electrons, which causes them to degrade in energy. The fact that heat i ...
MEASURING THE STARS
... The magnitude system Stellar surface temperature The spectral classificaGon of stars Hertzprung-‐Russel Diagram Stellar Luminosity Classes Stellar Radii ...
... The magnitude system Stellar surface temperature The spectral classificaGon of stars Hertzprung-‐Russel Diagram Stellar Luminosity Classes Stellar Radii ...
Gravitationally redshifted absorption lines in the x
... for 16 X-ray bursts from GS 1826-24. The three temperature phases are defined according to the spectral fits with the EPIC-pn data. An absorbed blackbody model is superimposed in red. The Ne x line at 12.1 (with 3.4 σ confidence) Å is included in the low-temperature spectrum. ...
... for 16 X-ray bursts from GS 1826-24. The three temperature phases are defined according to the spectral fits with the EPIC-pn data. An absorbed blackbody model is superimposed in red. The Ne x line at 12.1 (with 3.4 σ confidence) Å is included in the low-temperature spectrum. ...
Photometric variability of the Pre
... face. Some times the variability can be periodic due to long lived hot spots. This periodicity typically persists for only a couple of rotation cycles. The UXor type of variability is seen in HAEBE and some CTT stars from F-G spectral types. The typical amplitudes are of the order of 2-3 mag (V), an ...
... face. Some times the variability can be periodic due to long lived hot spots. This periodicity typically persists for only a couple of rotation cycles. The UXor type of variability is seen in HAEBE and some CTT stars from F-G spectral types. The typical amplitudes are of the order of 2-3 mag (V), an ...
![arXiv:1007.5481v1 [astro-ph.EP] 30 Jul 2010](http://s1.studyres.com/store/data/016640559_1-8bc20118c4d48efd5cfe1f2b10a85bec-300x300.png)
arXiv:1007.5481v1 [astro-ph.EP] 30 Jul 2010
... age between 0.12 and 3.15 Gyr. The lithium abundance of the star is consistent with its effective temperature, activity level, and age range derived from the stellar analysis. The density of the planet is extreme for its mass. It implies the existence of an amount of heavy elements with a mass betwe ...
... age between 0.12 and 3.15 Gyr. The lithium abundance of the star is consistent with its effective temperature, activity level, and age range derived from the stellar analysis. The density of the planet is extreme for its mass. It implies the existence of an amount of heavy elements with a mass betwe ...
Poster - unist
... evolution of GCs in the tidal fields, using N-body technique. As a result, we find that compact star clusters form under UV radiation fields and they are well consistent with the recognized correlation between velocity dispersion and mass for observed GCs. ...
... evolution of GCs in the tidal fields, using N-body technique. As a result, we find that compact star clusters form under UV radiation fields and they are well consistent with the recognized correlation between velocity dispersion and mass for observed GCs. ...
The Curtis-Shapley debate – two different views of
... In the mid-1920's using the 100 inch Hooker Telescope at Mount Wilson, then the largest telescope in the world, astronomer Edwin Hubble discovered Cepheid variable stars in the Andromeda Galaxy (M31). Hubble used these Cepheid variables to show that the distance to M31 was greater than even Shapley' ...
... In the mid-1920's using the 100 inch Hooker Telescope at Mount Wilson, then the largest telescope in the world, astronomer Edwin Hubble discovered Cepheid variable stars in the Andromeda Galaxy (M31). Hubble used these Cepheid variables to show that the distance to M31 was greater than even Shapley' ...
γ The Potential for Intensity Interferometry with –
... Photospheric absorption lines show Be stars are close to break-up rotational velocities. Also, Balmer line emission show gaseous circumstellar discs that appear and disappear on timescales of months to years. These two properties are somehow related, but have many open questions about the detailed p ...
... Photospheric absorption lines show Be stars are close to break-up rotational velocities. Also, Balmer line emission show gaseous circumstellar discs that appear and disappear on timescales of months to years. These two properties are somehow related, but have many open questions about the detailed p ...
Variability of Be stars
... • Discovery of 2 new Be stars, HD 4881 (V=6.2, B9 V) and HD 5839 (V=6.7, B9 V) (Miroshnichenko et al. 1999, MNRAS, 302, 612). • Periodic RV variations (84.3 d) of the emission peak and absorption wings of the H profile in Aquarii are discovered during the normal B-star phase (Bjorkman et al. 2002 ...
... • Discovery of 2 new Be stars, HD 4881 (V=6.2, B9 V) and HD 5839 (V=6.7, B9 V) (Miroshnichenko et al. 1999, MNRAS, 302, 612). • Periodic RV variations (84.3 d) of the emission peak and absorption wings of the H profile in Aquarii are discovered during the normal B-star phase (Bjorkman et al. 2002 ...
Stellar Astronomy Unit 3 Key Terms and Matching Definitions _____
... 7. A flattened galaxy reminiscent of a pinwheel. 8. An oval galaxy with no distinguishing spiral arms. 9. A collection of galaxies held together by their mutual gravitational attraction. 10. The collection of approximately 40 galaxies that includes the Milky Way Galaxy. 11. When two similarly-sized ...
... 7. A flattened galaxy reminiscent of a pinwheel. 8. An oval galaxy with no distinguishing spiral arms. 9. A collection of galaxies held together by their mutual gravitational attraction. 10. The collection of approximately 40 galaxies that includes the Milky Way Galaxy. 11. When two similarly-sized ...
Star
... Stars are evenly distributed in space Stars are clustered near the Sun We see all the stars in the Milky Way ...
... Stars are evenly distributed in space Stars are clustered near the Sun We see all the stars in the Milky Way ...
2015 SAO Summer Intern AAS Abstracts - Harvard
... This is a preliminary report on the mass of remaining hydrogen envelopes for stars massive enough to explode under core collapse. Using the stellar evolution code, MESA, our initial findings suggest that a significant fraction of massive stars with MZAMS = 20 − 60 Msun lose all but 10−3 Msun −10−1 M ...
... This is a preliminary report on the mass of remaining hydrogen envelopes for stars massive enough to explode under core collapse. Using the stellar evolution code, MESA, our initial findings suggest that a significant fraction of massive stars with MZAMS = 20 − 60 Msun lose all but 10−3 Msun −10−1 M ...
Lecture 6 - Stars and Distances
... Explained Werthimer, “if we had looked at the sky even a few seconds later we wouldn’t have found a match” for this candidate. A signal that drifts so quickly that it can only be heard for seconds at a time at a given frequency can only be detected by blind luck. Needless to say, such a transmission ...
... Explained Werthimer, “if we had looked at the sky even a few seconds later we wouldn’t have found a match” for this candidate. A signal that drifts so quickly that it can only be heard for seconds at a time at a given frequency can only be detected by blind luck. Needless to say, such a transmission ...
Hubblecast Episode 64: It All Ends with a Bang! — The incineration of
... discovered of this type. It is so far away that its light has taken more than 9 billion years to reach us — that’s about two thirds the age of the Universe. ...
... discovered of this type. It is so far away that its light has taken more than 9 billion years to reach us — that’s about two thirds the age of the Universe. ...
Planetary nebula
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.