Chapter 1-3
... of both stars vary, it is possible to accurately measure both the masses and radii (with 1–2 % accuracy in some cases) by fitting the radial-velocity curves and the eclipse lightcurve. Together with a photometric or, better, spectroscopic determination of T eff also the luminosity of such binaries c ...
... of both stars vary, it is possible to accurately measure both the masses and radii (with 1–2 % accuracy in some cases) by fitting the radial-velocity curves and the eclipse lightcurve. Together with a photometric or, better, spectroscopic determination of T eff also the luminosity of such binaries c ...
Planet formation Abstract Megan K Pickett and Andrew J Lim
... is from this disk that the planets somehow coalesced. Close to the forming Sun, where the temperatures were high enough to vaporize most volatiles, the terrestrial planets formed by the accumulation of silicon, iron, nickel and other refractory grains into progressively larger bodies. Far from the S ...
... is from this disk that the planets somehow coalesced. Close to the forming Sun, where the temperatures were high enough to vaporize most volatiles, the terrestrial planets formed by the accumulation of silicon, iron, nickel and other refractory grains into progressively larger bodies. Far from the S ...
azu_etd_13224_sip1_m
... an important source of disk atmosphere heating, and suggests that efficient H2 O formation and/or UV dissociation of N2 (both also associated with higher stellar accretion rates) may aid in the production of HCN. Studies following mine have further connected the abundance of HCN versus H2 O to the g ...
... an important source of disk atmosphere heating, and suggests that efficient H2 O formation and/or UV dissociation of N2 (both also associated with higher stellar accretion rates) may aid in the production of HCN. Studies following mine have further connected the abundance of HCN versus H2 O to the g ...
Document
... 1999: using ASCA, X-1 in M82 was found to vary by up to a factor of four, confirming that this bright source was indeed a single object. *Over half of ULXs are known to be variable, ruling out the multiple source or SNR hypothesis. ...
... 1999: using ASCA, X-1 in M82 was found to vary by up to a factor of four, confirming that this bright source was indeed a single object. *Over half of ULXs are known to be variable, ruling out the multiple source or SNR hypothesis. ...
W The X-Ray Universe X-ray images of the Universe are
... is so great that an X ray has a neg-ligible chance of getting to the ground. (The lower-energy visible-light photons interact weakly with the atmospheric atoms and pass through with little absorption.) In September 1949 a team led by Herbert Friedman of the Naval Research Laboratory was the first to ...
... is so great that an X ray has a neg-ligible chance of getting to the ground. (The lower-energy visible-light photons interact weakly with the atmospheric atoms and pass through with little absorption.) In September 1949 a team led by Herbert Friedman of the Naval Research Laboratory was the first to ...
Part I: Shining a Light on Visual Magnitude
... Qualitative analysis is fine, but what’s more interesting is to use STK with EOIR to quantitatively measure the brightness of these stars. Using metrics such as irradiance and detected signal we can estimate the visual magnitude of these stars, which will be the focus of this analysis. We’ll go into ...
... Qualitative analysis is fine, but what’s more interesting is to use STK with EOIR to quantitatively measure the brightness of these stars. Using metrics such as irradiance and detected signal we can estimate the visual magnitude of these stars, which will be the focus of this analysis. We’ll go into ...
astronomy advisory panel strategy
... In recent years, the study of galaxy formation and evolution has moved to position where they now incorporate enough of the relevant physics that they should allow the first meaningful tests of computer simulations against observational data, although is still limited by the huge dynamic ranges invo ...
... In recent years, the study of galaxy formation and evolution has moved to position where they now incorporate enough of the relevant physics that they should allow the first meaningful tests of computer simulations against observational data, although is still limited by the huge dynamic ranges invo ...
Here you can get a Science reprint
... system GRO J1655-40. The upper limit for the runaway kinetic energy of Cygnus X-1 is at least 20 times smaller than that estimated (3) for GRO J1655-40 and ⬃2 ⫻ 10⫺5 that of a SN of 1051 ergs. The kinematics of Cygnus X-1 and GRO J1655-40 suggest that the black holes in these two x-ray binaries were ...
... system GRO J1655-40. The upper limit for the runaway kinetic energy of Cygnus X-1 is at least 20 times smaller than that estimated (3) for GRO J1655-40 and ⬃2 ⫻ 10⫺5 that of a SN of 1051 ergs. The kinematics of Cygnus X-1 and GRO J1655-40 suggest that the black holes in these two x-ray binaries were ...
Hot subdwarf stars-galactic orbits and distribution perpendicular to
... The hotter subdwarf B (sdB) stars form a well defined group. Their luminosity is of the order of 10 L⊙ and their surface temperatures are roughly between 2 104 and 3 104 K. The age of the sdB stars does not follow from the stellar properties. The abundance of metals in subdwarf star atmospheres is p ...
... The hotter subdwarf B (sdB) stars form a well defined group. Their luminosity is of the order of 10 L⊙ and their surface temperatures are roughly between 2 104 and 3 104 K. The age of the sdB stars does not follow from the stellar properties. The abundance of metals in subdwarf star atmospheres is p ...
Andromeda Nebula Lies Outside Milky Way Galaxy
... Heber Curtis (left) and Harlow Shapley (right) Dr. Hubble's discovery settles the "Great Debate" over the size of our own Milky Way galaxy. It also settles the distance to spiral nebulae and what they are. Held on April 26, 1920 at the National Academy of Sciences in Washington, D.C., the debate foc ...
... Heber Curtis (left) and Harlow Shapley (right) Dr. Hubble's discovery settles the "Great Debate" over the size of our own Milky Way galaxy. It also settles the distance to spiral nebulae and what they are. Held on April 26, 1920 at the National Academy of Sciences in Washington, D.C., the debate foc ...
gateway - Thirty Meter Telescope
... How do dust and gas become stars and planets? Stars and planets form out of vast clouds of dust and gas. For reasons we don’t fully understand, areas of these clouds begin to collapse under gravity, forming protoplanetary disks, the infant stage of new solar systems. Astronomers will use TMT to dete ...
... How do dust and gas become stars and planets? Stars and planets form out of vast clouds of dust and gas. For reasons we don’t fully understand, areas of these clouds begin to collapse under gravity, forming protoplanetary disks, the infant stage of new solar systems. Astronomers will use TMT to dete ...
DUSTY CIRCUMSTELLAR DISKS B. Zuckerman
... Key Words stellar evolution, pre-main sequence, main sequence, red giants, white dwarfs ■ Abstract Dusty circumstellar disks in orbit around main-sequence stars were discovered in 1983 by the infrared astronomical satellite. It was the first time material that was not another star had been seen in o ...
... Key Words stellar evolution, pre-main sequence, main sequence, red giants, white dwarfs ■ Abstract Dusty circumstellar disks in orbit around main-sequence stars were discovered in 1983 by the infrared astronomical satellite. It was the first time material that was not another star had been seen in o ...
PDF only - at www.arxiv.org.
... 3. Center for Astrophysics and Space Astronomy, University of Colorado, ...
... 3. Center for Astrophysics and Space Astronomy, University of Colorado, ...
Additional Cosmology Images
... The sky is a jewelry box full of sparkling stars in these infrared images. The crown jewels are 14 massive stars on the verge of exploding as supernovae. These hefty stars reside in one of the most massive star clusters in the Milky Way. The bluish cluster is inside the white box in the large image ...
... The sky is a jewelry box full of sparkling stars in these infrared images. The crown jewels are 14 massive stars on the verge of exploding as supernovae. These hefty stars reside in one of the most massive star clusters in the Milky Way. The bluish cluster is inside the white box in the large image ...
15_Testbank
... 11) A 10-solar-mass star is about ten times more luminous than a 1-solar-mass star. Answer: FALSE 12) Most stars on the main sequence fuse hydrogen into helium in their cores, but some do not. Answer: FALSE 13) All stars spend approximately the same amount of time on the main sequence. Answer: FALS ...
... 11) A 10-solar-mass star is about ten times more luminous than a 1-solar-mass star. Answer: FALSE 12) Most stars on the main sequence fuse hydrogen into helium in their cores, but some do not. Answer: FALSE 13) All stars spend approximately the same amount of time on the main sequence. Answer: FALS ...
Calculating Parallax Lab
... One of the most difficult problems in astronomy is determining the distances to objects in the sky. There are four basic methods of determining distances: radar, parallax, standard candles, and the Hubble Law. Each of these methods is most useful at certain distances, with radar being useful nearby ...
... One of the most difficult problems in astronomy is determining the distances to objects in the sky. There are four basic methods of determining distances: radar, parallax, standard candles, and the Hubble Law. Each of these methods is most useful at certain distances, with radar being useful nearby ...
our knowledge of high-mass star formation at the dawn of - CEA-Irfu
... by Wolfire & Cassinelli (1987) by using the optical properties and composition of the mixture of dust grains proposed by Mathis et al. (1977). Assuming an accretion rate of 10−3 M⊙ yr−1 in a 100 M⊙ cloud, Wolfire & Cassinelli show that Γ is larger than one for any reasonable value of the radiation t ...
... by Wolfire & Cassinelli (1987) by using the optical properties and composition of the mixture of dust grains proposed by Mathis et al. (1977). Assuming an accretion rate of 10−3 M⊙ yr−1 in a 100 M⊙ cloud, Wolfire & Cassinelli show that Γ is larger than one for any reasonable value of the radiation t ...
The Gould Belt
... nebulae of the Gould belt. These are dwarfs in late spectral classes with masses of ≈ 1M⊙ and ages of several million years that have not reached the Main sequence stage. Stars have also been identified in terms of their emission in the HJ line, their lithium abundance, xray emission, position in the ...
... nebulae of the Gould belt. These are dwarfs in late spectral classes with masses of ≈ 1M⊙ and ages of several million years that have not reached the Main sequence stage. Stars have also been identified in terms of their emission in the HJ line, their lithium abundance, xray emission, position in the ...
The first carbon-enhanced metal-poor star found in the Sculptor
... spheroidal galaxies around the Milky Way. Here we present detailed abundances from ESO VLT/UVES high-resolution spectroscopy for ET0097, the first CEMP star found in the Sculptor dwarf spheroidal, which is one of the best studied dwarf galaxies in the Local Group. This star has [Fe/H] = −2.03 ± 0.10 ...
... spheroidal galaxies around the Milky Way. Here we present detailed abundances from ESO VLT/UVES high-resolution spectroscopy for ET0097, the first CEMP star found in the Sculptor dwarf spheroidal, which is one of the best studied dwarf galaxies in the Local Group. This star has [Fe/H] = −2.03 ± 0.10 ...
File
... Describe the methods scientists have used to help with this search in both our Solar System and the rest of the Universe. ...
... Describe the methods scientists have used to help with this search in both our Solar System and the rest of the Universe. ...
Widener University
... 1028 W. The star is initially composed of 100% H and converts all of it to He, each chain of 4H He releasing an amount of energy E = 4.3 x 10-12 J. Calculate: a) the total number of H nuclei (protons) present in the entire star. b) the total number of 4H He chains available, based on the result ...
... 1028 W. The star is initially composed of 100% H and converts all of it to He, each chain of 4H He releasing an amount of energy E = 4.3 x 10-12 J. Calculate: a) the total number of H nuclei (protons) present in the entire star. b) the total number of 4H He chains available, based on the result ...
RApid Temporal Survey-RATS I: Overview and first results
... The intensity of stellar objects can vary on a wide range of time-scales, ranging from seconds to months to years. A large number of projects now exist whose aim is to detect such varying sources. The reasons for this are many, but include the search for extra-solar planets and interacting binary st ...
... The intensity of stellar objects can vary on a wide range of time-scales, ranging from seconds to months to years. A large number of projects now exist whose aim is to detect such varying sources. The reasons for this are many, but include the search for extra-solar planets and interacting binary st ...