Explosion and remnants of massive stars
... remnant is left. The lightcurve of a Type Ia supernova is powered by the radioactive decay of the 56 Ni formed in the explosion. The nickel mass is a substantial fraction of the mass of the white dwarf, 0.5 − 1.0 M⊙ , which is the main reason for the greater peak luminosities of SNe Ia compared to m ...
... remnant is left. The lightcurve of a Type Ia supernova is powered by the radioactive decay of the 56 Ni formed in the explosion. The nickel mass is a substantial fraction of the mass of the white dwarf, 0.5 − 1.0 M⊙ , which is the main reason for the greater peak luminosities of SNe Ia compared to m ...
Draco: The Dragon - Courtney Stookey
... constellation. The star is referred to as ‘the serpent’. This is an orange giant that is about 148 light years distant. While Eltanin is the brightest star in the constellation, Thuban, or 3445 alpha Draconis, is not very noticeable in comparison. This star is referred to as ‘the basilisk’. Thuban i ...
... constellation. The star is referred to as ‘the serpent’. This is an orange giant that is about 148 light years distant. While Eltanin is the brightest star in the constellation, Thuban, or 3445 alpha Draconis, is not very noticeable in comparison. This star is referred to as ‘the basilisk’. Thuban i ...
Spiral structure of the Third Galactic Quadrant and the solution to the
... exhibit clear post main-sequence signatures expected for a 4-10 Gyr population (Martı́nez-Delgado et al. 2005) (red clump or red giant branch, horizontal branch, RR-Lyrae), a distinctive feature, popularised as the Blue Plume (BP; see Fig. 1) has been taken as strong evidence for the existence of th ...
... exhibit clear post main-sequence signatures expected for a 4-10 Gyr population (Martı́nez-Delgado et al. 2005) (red clump or red giant branch, horizontal branch, RR-Lyrae), a distinctive feature, popularised as the Blue Plume (BP; see Fig. 1) has been taken as strong evidence for the existence of th ...
Herschel
... with a ~100 UA, e ~0.3, Tdust ~ 40 K, Ldust/L* ≈ 10-5 Asymmetry: Caused by a planet?. (Eiroa et al., 2010, A&A, 518, L131, Thebault et al., Faramaz et al., 2014, A&A, 563, 72) ...
... with a ~100 UA, e ~0.3, Tdust ~ 40 K, Ldust/L* ≈ 10-5 Asymmetry: Caused by a planet?. (Eiroa et al., 2010, A&A, 518, L131, Thebault et al., Faramaz et al., 2014, A&A, 563, 72) ...
Document
... A majority of the galaxies in rich clusters are ellipticals, not spirals. There is often a single, very large central elliptical galaxy (sometimes two) that is cannibalizing other galaxies in its vicinity, growing bigger with time (see figure, top). X-ray observations of rich clusters reveal a hot i ...
... A majority of the galaxies in rich clusters are ellipticals, not spirals. There is often a single, very large central elliptical galaxy (sometimes two) that is cannibalizing other galaxies in its vicinity, growing bigger with time (see figure, top). X-ray observations of rich clusters reveal a hot i ...
Early Star-Forming Galaxies and the Reionisation of the Universe
... (wavelength λ<91.2 nm) generated by primitive stars and galaxies4 (Fig. 1). Astronomers wish to confirm the connection between early galaxies and reionisation because detailed studies of this period of cosmic history will reveal the physical processes that originally shaped the galaxies of various l ...
... (wavelength λ<91.2 nm) generated by primitive stars and galaxies4 (Fig. 1). Astronomers wish to confirm the connection between early galaxies and reionisation because detailed studies of this period of cosmic history will reveal the physical processes that originally shaped the galaxies of various l ...
What is a standard candle?
... second 50 light years from Earth are discovered. How much fainter does the farther star appear to be? A. square root of 10 B. 10 C. 100 D. 1,000 E. the farther star does not appear fainter, since it is ...
... second 50 light years from Earth are discovered. How much fainter does the farther star appear to be? A. square root of 10 B. 10 C. 100 D. 1,000 E. the farther star does not appear fainter, since it is ...
Presentation - Relativity Group
... • How can we learn about the lives of stars, which last millions to billions of years? • By taking observations of many stars, we can study stars in many phases of life, just as we might study how humans age by observing the humans living in a village at one time. • What two basic physical propertie ...
... • How can we learn about the lives of stars, which last millions to billions of years? • By taking observations of many stars, we can study stars in many phases of life, just as we might study how humans age by observing the humans living in a village at one time. • What two basic physical propertie ...
December - Weasner
... send that boat to the celestial breaker’s yard, on the grounds that it was too unwieldy. Despite being thought of as a far-southern group, I was able to hunt out a variety of targets from Northern England ! M47 was a large grouping of some 25 brighter stars which showed up well despite the Full Moon ...
... send that boat to the celestial breaker’s yard, on the grounds that it was too unwieldy. Despite being thought of as a far-southern group, I was able to hunt out a variety of targets from Northern England ! M47 was a large grouping of some 25 brighter stars which showed up well despite the Full Moon ...
Galaxies: Interactions and Mergers Encyclopedia of Astronomy & Astrophysics eaa.iop.org C Mihos
... prone to early bar formation, inflow and central activity. Similarly, galaxies in which the disk contributes little to the dynamical mass (e.g. low surface brightness disk galaxies) will also be more resistive to inflow, as the self-gravity of the disk is much weaker. Of course, in any case the gala ...
... prone to early bar formation, inflow and central activity. Similarly, galaxies in which the disk contributes little to the dynamical mass (e.g. low surface brightness disk galaxies) will also be more resistive to inflow, as the self-gravity of the disk is much weaker. Of course, in any case the gala ...
PDF file - Memorie della SAIt
... a fossil record of the nucleosynthesis that occurred several Gyr ago in halo AGB stars. They are dwarfs or giants, whose surface composition was polluted by the wind of an AGB companion. Then, the C and s-element enhancements are ashes of the nucleosynthesis occurred in the He-rich inter-shell of a ...
... a fossil record of the nucleosynthesis that occurred several Gyr ago in halo AGB stars. They are dwarfs or giants, whose surface composition was polluted by the wind of an AGB companion. Then, the C and s-element enhancements are ashes of the nucleosynthesis occurred in the He-rich inter-shell of a ...
Neutron Stars and Black Holes
... second 50 light years from Earth are discovered. How much fainter does the farther star appear to be? A. square root of 10 B. 10 C. 100 D. 1,000 E. the farther star does not appear fainter, since it is ...
... second 50 light years from Earth are discovered. How much fainter does the farther star appear to be? A. square root of 10 B. 10 C. 100 D. 1,000 E. the farther star does not appear fainter, since it is ...
Ultra faint dwarfs: probing early cosmic star formation
... mixed merging of star-forming and starless progenitors; they are typically more massive than gas-rich haloes and form at lower redshifts. Their smaller baryonic content is the result of shock-heating of the infalling gas during major merging events (Cox et al. 2004) which stops accretion. Finally, g ...
... mixed merging of star-forming and starless progenitors; they are typically more massive than gas-rich haloes and form at lower redshifts. Their smaller baryonic content is the result of shock-heating of the infalling gas during major merging events (Cox et al. 2004) which stops accretion. Finally, g ...
Astronomy Astrophysics
... Such collisions are, however, likely the only means of forcing much of the gas out of the inner regions of spirals because tidal forces primarily affect the less bound external regions. The stars are not affected by collisions of the ISMs of the galaxies and of course stars do not collide with each ot ...
... Such collisions are, however, likely the only means of forcing much of the gas out of the inner regions of spirals because tidal forces primarily affect the less bound external regions. The stars are not affected by collisions of the ISMs of the galaxies and of course stars do not collide with each ot ...
The age structure of the Milky Way`s halo
... that are in the process of being accreted by the Milky Way, such as the Sagittarius Stream16 and the Orphan Stream17, also possess distinct metallicities and kinematics. The integrated contribution from these debris streams may comprise as much as half of the stars now found in the halo system18. In ...
... that are in the process of being accreted by the Milky Way, such as the Sagittarius Stream16 and the Orphan Stream17, also possess distinct metallicities and kinematics. The integrated contribution from these debris streams may comprise as much as half of the stars now found in the halo system18. In ...
Goal: To understand clusters of stars
... old. • And the cluster is moving by us at 46 km/s. • 46 km/s = 1 light year per 6000 years ...
... old. • And the cluster is moving by us at 46 km/s. • 46 km/s = 1 light year per 6000 years ...
Goal: To understand clusters of stars
... old. • And the cluster is moving by us at 46 km/s. • 46 km/s = 1 light year per 6000 years ...
... old. • And the cluster is moving by us at 46 km/s. • 46 km/s = 1 light year per 6000 years ...
in search of antimatter in the universe
... to collide with a star, the remnant of a star (such as a Planetary nebula or a supernova remnant), or a molecular cloud, then the particles in the jet would collide with the particles of the body, and slow down. Once a particle has undergone enough collisions, and has less energy than the ionisation ...
... to collide with a star, the remnant of a star (such as a Planetary nebula or a supernova remnant), or a molecular cloud, then the particles in the jet would collide with the particles of the body, and slow down. Once a particle has undergone enough collisions, and has less energy than the ionisation ...
A near IR adaptive optics search for faint companions to early
... We suspect that it is a highly reddened (J − K = 2.4) background star. In this region of sky there are other multiple systems with similar proper motions and radial velocities (e.g. HR 3283, 3322, 3359). Therefore, NO Pup belongs to an association. HD 108248/49/50 = α1,2 Cru. The coronographic image ...
... We suspect that it is a highly reddened (J − K = 2.4) background star. In this region of sky there are other multiple systems with similar proper motions and radial velocities (e.g. HR 3283, 3322, 3359). Therefore, NO Pup belongs to an association. HD 108248/49/50 = α1,2 Cru. The coronographic image ...
P - Inaf
... molecular); (3) the presence of any outflowing gas that is lost recycled), which can be approximated as being proportional to mass loading factor , defined as Moutflow = SFR (note that if account only for the fraction of gas that is lost, i.e. it is an “effe ...
... molecular); (3) the presence of any outflowing gas that is lost recycled), which can be approximated as being proportional to mass loading factor , defined as Moutflow = SFR (note that if account only for the fraction of gas that is lost, i.e. it is an “effe ...
egg nebula - IOPscience
... The origin of the equatorial H2 emission is a puzzle, although the fact that its radial extent is almost identical to that of the polar spindles strongly suggests a common origin for the polar and equatorial structures. The H2 emission spectrum implies that both the equatorial and polar H2 emission ...
... The origin of the equatorial H2 emission is a puzzle, although the fact that its radial extent is almost identical to that of the polar spindles strongly suggests a common origin for the polar and equatorial structures. The H2 emission spectrum implies that both the equatorial and polar H2 emission ...
Colliding molecular clouds in head
... between the interstellar media (ISMs) of the galaxies. We show that collisions between molecular clouds bring H2 into the bridge region. Although the dense clouds are ionized by the collisions, they cool and recombine very quickly and become molecular again even before the galactic disks separate. B ...
... between the interstellar media (ISMs) of the galaxies. We show that collisions between molecular clouds bring H2 into the bridge region. Although the dense clouds are ionized by the collisions, they cool and recombine very quickly and become molecular again even before the galactic disks separate. B ...
Proto-planetary disks
... Grains emit: • efficiently at short wavelengths λD: Qem = (D/λ)n
Observations at different wavelengths:
• probe different dust sizes
• tell us about the size distribution
Rule of thumb:
• λ<100µm probes smallest (few µm) grains
• λ>100µm probes ...
... Grains emit: • efficiently at short wavelengths λ
3.2 Spectra and Spectral Classification
... - resolution of detector (pixel size) - width of the entrance slit … must be optimized Diffraction grating Camera mirror ...
... - resolution of detector (pixel size) - width of the entrance slit … must be optimized Diffraction grating Camera mirror ...
KINEMATIC DISCOVERY OF A STELLAR STREAM LOCATED IN
... (0 < log g < 4.0) from the Sloan Digital Sky Survey Data Release 8 (SDSS DR8) spectroscopic data in the south Galactic hemisphere. The Cetus stream was clearly present in velocity versus Galactic latitude plots of these stars, along with an additional feature consisting of a few stars clumped at vgs ...
... (0 < log g < 4.0) from the Sloan Digital Sky Survey Data Release 8 (SDSS DR8) spectroscopic data in the south Galactic hemisphere. The Cetus stream was clearly present in velocity versus Galactic latitude plots of these stars, along with an additional feature consisting of a few stars clumped at vgs ...
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.