• Teacher developed presentations. • Teacher developed laboratory
... CCSS.ELA-Literacy.WHST.9-10.2b Develop the topic with well-chosen, relevant, and sufficient facts, extended definitions, concrete details, quotations, or other information and examples appropriate to the audience’s knowledge of the topic. CCSS.ELA-Literacy.WHST.9-10.2c Use varied transitions and sen ...
... CCSS.ELA-Literacy.WHST.9-10.2b Develop the topic with well-chosen, relevant, and sufficient facts, extended definitions, concrete details, quotations, or other information and examples appropriate to the audience’s knowledge of the topic. CCSS.ELA-Literacy.WHST.9-10.2c Use varied transitions and sen ...
Cycles of magnetic activity in solar-type stars. The place of the Sun
... with different levels of the chromospheric and coronal activity confirms that the Sun belongs to stars with the low level of the chromospheric activity and stands apart among these stars by the minimum level of the coronal radiation and minimum flux variations of the photospheric radiation. Key words: ...
... with different levels of the chromospheric and coronal activity confirms that the Sun belongs to stars with the low level of the chromospheric activity and stands apart among these stars by the minimum level of the coronal radiation and minimum flux variations of the photospheric radiation. Key words: ...
Lecture 3
... Lecture Summary • LBGs at z>4 are significantly harder to find than those at z<4 • LBGs at z~6 are a lot harder than z~5 • The sample looked at varies with survey filters and characteristics • Lyman- emission can affect measured magnitudes and galaxy selection • With increasing redshift see: ...
... Lecture Summary • LBGs at z>4 are significantly harder to find than those at z<4 • LBGs at z~6 are a lot harder than z~5 • The sample looked at varies with survey filters and characteristics • Lyman- emission can affect measured magnitudes and galaxy selection • With increasing redshift see: ...
discovery of four new massive and dense cold cores
... regions of molecular gas with distinctive physical parameters, which we refer to as massive dense cores.1 For example, from observations of the CS (5 ! 4) line emission toward massive star–forming regions associated with H2O masers, Plume et al. (1997) derived typical radii of 0.5 pc, densities of 8 ...
... regions of molecular gas with distinctive physical parameters, which we refer to as massive dense cores.1 For example, from observations of the CS (5 ! 4) line emission toward massive star–forming regions associated with H2O masers, Plume et al. (1997) derived typical radii of 0.5 pc, densities of 8 ...
Aldebaran
... Aldebaran started off as a large, relatively cool mass of gas, part of a nebula. As gravity caused the gas to contract, its temperature rose, eventually becoming high enough to trigger a nuclear reaction in its atoms. When the gases and dust of the nebula contracted, a protostar was formed. Gravity ...
... Aldebaran started off as a large, relatively cool mass of gas, part of a nebula. As gravity caused the gas to contract, its temperature rose, eventually becoming high enough to trigger a nuclear reaction in its atoms. When the gases and dust of the nebula contracted, a protostar was formed. Gravity ...
Statistical analysis of stellar evolution
... of plasma. If the mass of the resulting protostar exceeds about 10% of the mass of the Sun, M , its core will ignite in a thermonuclear reaction that is powered by the fusion of hydrogen into helium. This reaction at the star’s core can continue for millions or billions of years depending on the or ...
... of plasma. If the mass of the resulting protostar exceeds about 10% of the mass of the Sun, M , its core will ignite in a thermonuclear reaction that is powered by the fusion of hydrogen into helium. This reaction at the star’s core can continue for millions or billions of years depending on the or ...
3.1 Radio Astronomy Research Results For much of PY 2010, radio
... An AGES objective is to investigate the number of low mass gas rich dwarf galaxies that reside around isolated galaxies and within galaxy groups, as hierarchical models of galaxy formation predict hundreds of dwarf companions for each giant galaxy. AGES typically finds only one or two new dwarf gala ...
... An AGES objective is to investigate the number of low mass gas rich dwarf galaxies that reside around isolated galaxies and within galaxy groups, as hierarchical models of galaxy formation predict hundreds of dwarf companions for each giant galaxy. AGES typically finds only one or two new dwarf gala ...
Star 1 A star is a massive, luminous ball of plasma held together by
... Astronomical Union (IAU).[42] A number of private companies sell names of stars, which the British Library calls an unregulated commercial enterprise.[43] [44] However, the IAU has disassociated itself from this commercial practice, and these names are neither recognized by the IAU nor used by them. ...
... Astronomical Union (IAU).[42] A number of private companies sell names of stars, which the British Library calls an unregulated commercial enterprise.[43] [44] However, the IAU has disassociated itself from this commercial practice, and these names are neither recognized by the IAU nor used by them. ...
structure and evolution of white dwarfs and their
... Theoretical and observational study of stellar evolution has placed white dwarfs as one possible end point of the process. In general terms, all stars with masses below about eight times that of the Sun will pass through one or more red giant phases before losing most of their original mass to form ...
... Theoretical and observational study of stellar evolution has placed white dwarfs as one possible end point of the process. In general terms, all stars with masses below about eight times that of the Sun will pass through one or more red giant phases before losing most of their original mass to form ...
Oxygen and Neon Abundances of B-Type Stars in Comparison with
... current Galactic gas and in the solar atmosphere (i.e., the former being appreciably lower by 0.3 dex), apparently contradicting the Galactic chemical evolution, we carried out oxygen abundance determinations for 64 mid- through late-B stars by using the O I 6156–8 lines while taking into account ...
... current Galactic gas and in the solar atmosphere (i.e., the former being appreciably lower by 0.3 dex), apparently contradicting the Galactic chemical evolution, we carried out oxygen abundance determinations for 64 mid- through late-B stars by using the O I 6156–8 lines while taking into account ...
Indications for an influence of Hot Jupiters
... Gyr) from Micela et al. (1997). We use the median X-ray luminosities and standard deviations from those authors; if no standard deviation is given, we fit the measured luminosities with a log-normal distribution to derive the median and the standard deviation. The literature gives values for the chr ...
... Gyr) from Micela et al. (1997). We use the median X-ray luminosities and standard deviations from those authors; if no standard deviation is given, we fit the measured luminosities with a log-normal distribution to derive the median and the standard deviation. The literature gives values for the chr ...
Hubble Space Telescope Imaging of Post
... gas-rich and morphologically disk-dominated. Whereas, the red sequence population is typically quiescent, gas-poor and morphologically spheroidal. Since z = 1 the stellar mass contained within the red sequence has doubled while that of the blue cloud remains more or less constant. Some blue cloud ga ...
... gas-rich and morphologically disk-dominated. Whereas, the red sequence population is typically quiescent, gas-poor and morphologically spheroidal. Since z = 1 the stellar mass contained within the red sequence has doubled while that of the blue cloud remains more or less constant. Some blue cloud ga ...
Summary of Dynamics of the regular hendecagon: N = 11
... It makes sense that the points adjacent to D[1] will have similar step sequences. The first 20 corner indices for a point close to p0 are {11,5,10,4,9,3,8,1,6,11,5,10,4,9,2,7,1,6,11,5} and it is clear they advance by {5,5,5,5,5,5,4} (mod 11), but of course this sequence will eventually break down. C ...
... It makes sense that the points adjacent to D[1] will have similar step sequences. The first 20 corner indices for a point close to p0 are {11,5,10,4,9,3,8,1,6,11,5,10,4,9,2,7,1,6,11,5} and it is clear they advance by {5,5,5,5,5,5,4} (mod 11), but of course this sequence will eventually break down. C ...
The new X-ray universe
... of sources) and at the known distance of M82 this implied that it was “ultraluminous” (Lx >1039 erg s–1; the source in M82 varies up 1041 erg s–1). While the existence of such objects was hinted at by earlier missions, a substantial number have now been found in Chandra and XMM observations of nearb ...
... of sources) and at the known distance of M82 this implied that it was “ultraluminous” (Lx >1039 erg s–1; the source in M82 varies up 1041 erg s–1). While the existence of such objects was hinted at by earlier missions, a substantial number have now been found in Chandra and XMM observations of nearb ...
The Jansky Very Large Array – New Capabilities, New Science
... observations as well as VLA. • The rise of ALMA will strengthen this complementarity, with stellar scientific results. • New example – Wagg and Carilli combine VLA and ALMA for early forming galaxies: – Massive galaxies at z~2 must have formed at earlier epochs. – Formation phase seems to have been ...
... observations as well as VLA. • The rise of ALMA will strengthen this complementarity, with stellar scientific results. • New example – Wagg and Carilli combine VLA and ALMA for early forming galaxies: – Massive galaxies at z~2 must have formed at earlier epochs. – Formation phase seems to have been ...
H 2 O, OH, SiO, NH 3 and CH 3 OH
... [proh-toh-stahr] an early stage in the evolution of a star, after the beginning of the collapse of the gas cloud from which it is formed, but before sufficient contraction has occurred to permit initiation of nuclear reactions at its core. ...
... [proh-toh-stahr] an early stage in the evolution of a star, after the beginning of the collapse of the gas cloud from which it is formed, but before sufficient contraction has occurred to permit initiation of nuclear reactions at its core. ...
High-precision abundances of elements in solar twin stars: Trends
... (EWs) of spectral lines by Gaussian fitting relative to pseudocontinuum regions lying within 3 Å from the line measured. These regions do not necessarily represent the true continuum, but care was taken to use the same continuum windows in all stars, so that differences in EW between stars are preci ...
... (EWs) of spectral lines by Gaussian fitting relative to pseudocontinuum regions lying within 3 Å from the line measured. These regions do not necessarily represent the true continuum, but care was taken to use the same continuum windows in all stars, so that differences in EW between stars are preci ...
the chandra deep field–north survey. xvii. evolution of
... The X-ray data utilized here are part of the 2 Ms CDF-N survey obtained with the Advanced CCD Imaging Spectrometer (ACIS) detector on board the Chandra X-Ray Observatory. The satellite and detector are described by Weisskopf et al. (2002). Extragalactic results from the CDF-N project are described i ...
... The X-ray data utilized here are part of the 2 Ms CDF-N survey obtained with the Advanced CCD Imaging Spectrometer (ACIS) detector on board the Chandra X-Ray Observatory. The satellite and detector are described by Weisskopf et al. (2002). Extragalactic results from the CDF-N project are described i ...
Mergers of massive main sequence binaries
... we analyzed a grid of binary SMC models computed by De Mink et al. (2007) which allowed us to calculate the hydrogen fraction of the merger star, which we shall discuss in Sect. 3.3. We considered the third question by simulating a cluster of stars with SMC metallicity (Sect. 4) which formed instant ...
... we analyzed a grid of binary SMC models computed by De Mink et al. (2007) which allowed us to calculate the hydrogen fraction of the merger star, which we shall discuss in Sect. 3.3. We considered the third question by simulating a cluster of stars with SMC metallicity (Sect. 4) which formed instant ...
When we look at a neighboring galaxy (such as M31, the
... physically larger, but less massive, than our Milky Way Galaxy. The Andromeda is the largest member of the Local Group, a cluster of about 30 galaxies that are gravitationally attracted to one another. At a distance of 2.5 million light-years, it is the most distant object easily seen with the unaid ...
... physically larger, but less massive, than our Milky Way Galaxy. The Andromeda is the largest member of the Local Group, a cluster of about 30 galaxies that are gravitationally attracted to one another. At a distance of 2.5 million light-years, it is the most distant object easily seen with the unaid ...
Annual Report 2012 - Max Planck Institute for Astrophysics
... instrumental activities carried out in other MaxPlanck institutes. From its inception the MPA has The Max-Planck-Institut für Astrophysik, called had an internationally-recognized numerical astrothe MPA for short, was founded in 1958 under the physics program that is unparalleled by any other direct ...
... instrumental activities carried out in other MaxPlanck institutes. From its inception the MPA has The Max-Planck-Institut für Astrophysik, called had an internationally-recognized numerical astrothe MPA for short, was founded in 1958 under the physics program that is unparalleled by any other direct ...
Spiral arm structures revealed in the M31 galaxy
... Striking regularities are found in the northwestern arm of the M31 galaxy. Star complexes located in this arm are spaced 1.2 kpc apart and have similar sizes of about 0.6 kpc. This pattern is observed within the arm region where Beck et al. (1989) detected a strong regular magnetic field with the wa ...
... Striking regularities are found in the northwestern arm of the M31 galaxy. Star complexes located in this arm are spaced 1.2 kpc apart and have similar sizes of about 0.6 kpc. This pattern is observed within the arm region where Beck et al. (1989) detected a strong regular magnetic field with the wa ...
ULXs: General Properties and Variability - X
... also occur in dwarfs and in elliptical galaxies with little present day star formationin ellipticals the maximal luminosity is 1040 ergs/sec In NGC720 a nearby giant elliptical with no star formation the number of ULXs is comparable to that of active star forming galaxies (Jeltema et al 2003)-at lea ...
... also occur in dwarfs and in elliptical galaxies with little present day star formationin ellipticals the maximal luminosity is 1040 ergs/sec In NGC720 a nearby giant elliptical with no star formation the number of ULXs is comparable to that of active star forming galaxies (Jeltema et al 2003)-at lea ...
Non-thermal hard X-ray emission from stellar coronae
... radiation, winds, and energetic particles originating from the central star ⇒ heating, ionization, evaporation How is planetary formation affected? ...
... radiation, winds, and energetic particles originating from the central star ⇒ heating, ionization, evaporation How is planetary formation affected? ...
Research Papers-Cosmology/Download/6307
... directly from the observations, is a spiral galaxy in which stars visualized the boundary of the core of the vortex of the dark gas. The observations show that the stars in the nucleus of the spiral galaxies rotate around a common center under the law of the rotation of a rigid body and only the sta ...
... directly from the observations, is a spiral galaxy in which stars visualized the boundary of the core of the vortex of the dark gas. The observations show that the stars in the nucleus of the spiral galaxies rotate around a common center under the law of the rotation of a rigid body and only the sta ...
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.