Stellar Properties
... • a star could be very bright because is was very close to us; not because it was truly bright • two stars in the same constellation might not be close to each other; one could be much farther away ...
... • a star could be very bright because is was very close to us; not because it was truly bright • two stars in the same constellation might not be close to each other; one could be much farther away ...
BSA Astronomy Merit Badge
... Remove wet clothing. If the person is wearing wet clothing, remove it. Cut away clothing if necessary to avoid excessive movement. Cover the person with blankets. Use layers of dry blankets or coats to warm the person. Cover the person's head, leaving only the face exposed. Insulate the person's bod ...
... Remove wet clothing. If the person is wearing wet clothing, remove it. Cut away clothing if necessary to avoid excessive movement. Cover the person with blankets. Use layers of dry blankets or coats to warm the person. Cover the person's head, leaving only the face exposed. Insulate the person's bod ...
Spiral structure of the Third Galactic Quadrant and the solution to the
... Fig. 1) has been taken as strong evidence for the existence of the CMa galaxy (Bellazzini et al. 2004; Dinescu et al. 2005; Martı́nez-Delgado et al. 2005). The BP has been modelled and interpreted as the last burst of star formation in that galaxy 1-2 Gyr ago (which, given that it is a 1-2 Gyr popul ...
... Fig. 1) has been taken as strong evidence for the existence of the CMa galaxy (Bellazzini et al. 2004; Dinescu et al. 2005; Martı́nez-Delgado et al. 2005). The BP has been modelled and interpreted as the last burst of star formation in that galaxy 1-2 Gyr ago (which, given that it is a 1-2 Gyr popul ...
Small star patterns for telescopes and binoculars Demelza Ramakers
... the middle of this jewel sparkle a few stars. I found it hard to find this asterism, because there are a lot of stars visible in this area. I concentrated at finding a few double stars that are closely together. That’s how I found The Fairy Ring. Actually: to me the name Chaple’s Arc sounds more app ...
... the middle of this jewel sparkle a few stars. I found it hard to find this asterism, because there are a lot of stars visible in this area. I concentrated at finding a few double stars that are closely together. That’s how I found The Fairy Ring. Actually: to me the name Chaple’s Arc sounds more app ...
Searching for RR Lyrae Stars in M15
... the light curves well-resemble that of a sinusoid. RRab stars pulsate in the fundamental radial mode while RRc stars pulsate in the first overtone radial mode. In the fundamental radial mode, the gases move in the same direction at every point in the star [1]. In the first overtone radial mode, the ...
... the light curves well-resemble that of a sinusoid. RRab stars pulsate in the fundamental radial mode while RRc stars pulsate in the first overtone radial mode. In the fundamental radial mode, the gases move in the same direction at every point in the star [1]. In the first overtone radial mode, the ...
Section 2
... in the winter sky is named Orion, the Hunter, after a Greek myth. In this constellation, Orion is seen with a sword in his belt and an upraised arm. The ancient Sumerians thought that the stars in Orion formed the outline of a sheep. In ancient China, this group of stars was called “three,” probably ...
... in the winter sky is named Orion, the Hunter, after a Greek myth. In this constellation, Orion is seen with a sword in his belt and an upraised arm. The ancient Sumerians thought that the stars in Orion formed the outline of a sheep. In ancient China, this group of stars was called “three,” probably ...
PPT - ALFALFA survey
... Schneider (2000). It was a drift-scan survey taken in a series of declination strips with the Arecibo 305-m telescope. The velocity limit of the ADBS is 8000 km/s (it is volume limited!). The full ADBS sample includes 265 galaxies over ~420 sq. deg. • Since it is a “blind” HI survey, it does not suf ...
... Schneider (2000). It was a drift-scan survey taken in a series of declination strips with the Arecibo 305-m telescope. The velocity limit of the ADBS is 8000 km/s (it is volume limited!). The full ADBS sample includes 265 galaxies over ~420 sq. deg. • Since it is a “blind” HI survey, it does not suf ...
Infrared Properties of Star-Forming Dwarf Galaxies. I. Dwarf Irregular
... in total) during which we observed 34 field dwarfs in the NIR. Of these, a total of about 12 nights were used to observe the field dIs. The remaining 15 nights were dedicated to BCDs in the Virgo Cluster. All allocated observing time was bright (the Moon was within 5 days of full). Our observations ...
... in total) during which we observed 34 field dwarfs in the NIR. Of these, a total of about 12 nights were used to observe the field dIs. The remaining 15 nights were dedicated to BCDs in the Virgo Cluster. All allocated observing time was bright (the Moon was within 5 days of full). Our observations ...
Table of Contents - Shawnee State University
... The Orion Educator’s Guide is designed for Planetarians, Teachers, and parents. The information is researched, organized, and laid out so that the educator need not spend hours coming up with lesson plans or labs. This has already been accomplished by certified educators. The guide is written to all ...
... The Orion Educator’s Guide is designed for Planetarians, Teachers, and parents. The information is researched, organized, and laid out so that the educator need not spend hours coming up with lesson plans or labs. This has already been accomplished by certified educators. The guide is written to all ...
1 Introduction - High Point University
... Table 6: Fill in the empty fields above. 3. Check show luminosity classes and show isoradius lines (if they are not already checked). The green region (Dwarfs (V)) is known as the main sequence and contains all stars that are fusing hydrogen into helium as their primary energy source. Over 90% of al ...
... Table 6: Fill in the empty fields above. 3. Check show luminosity classes and show isoradius lines (if they are not already checked). The green region (Dwarfs (V)) is known as the main sequence and contains all stars that are fusing hydrogen into helium as their primary energy source. Over 90% of al ...
The new Basel high-latitude field star survey of the Galaxy
... distance R ∼ 7.3 kpc and radial abundance gradient ∂[M/H]/∂x = −0.078 ± 0.016 dex/kpc, and a thick disk with mean metallicity h[M/H]i = −0.73±0.15 dex and vertical metallicity gradient ∂[M/H]/∂z = −0.07±0.03 dex/kpc. Any radial gradient of the thick disk is shown to be marginal, 0 ≥ ∂[M/H]/∂x ≥ −0.0 ...
... distance R ∼ 7.3 kpc and radial abundance gradient ∂[M/H]/∂x = −0.078 ± 0.016 dex/kpc, and a thick disk with mean metallicity h[M/H]i = −0.73±0.15 dex and vertical metallicity gradient ∂[M/H]/∂z = −0.07±0.03 dex/kpc. Any radial gradient of the thick disk is shown to be marginal, 0 ≥ ∂[M/H]/∂x ≥ −0.0 ...
Early Star-Forming Galaxies
... Rodighiero used Herschel ’s far-infrared camera to look for galaxies hidden from visible-light observations because of their intervening dust. This allowed the astronomers to assemble a more complete picture of star birth than ever before. The team targeted two well-known regions of the sky that ha ...
... Rodighiero used Herschel ’s far-infrared camera to look for galaxies hidden from visible-light observations because of their intervening dust. This allowed the astronomers to assemble a more complete picture of star birth than ever before. The team targeted two well-known regions of the sky that ha ...
Teacher`s Guide - Cornell Science Inquiry Partnerships
... Stars are a subject that students often struggle to understand. How can astronomers possibly come to know the physical properties of stars when they are so far away? And how do we learn anything about the way stars evolve in time when it takes billions of years for most of them to change significant ...
... Stars are a subject that students often struggle to understand. How can astronomers possibly come to know the physical properties of stars when they are so far away? And how do we learn anything about the way stars evolve in time when it takes billions of years for most of them to change significant ...
Staring Back to Cosmic Dawn - UC-HiPACC
... But at cosmic high noon, when stars were blazing into existence at peak rates, many galaxies look distorted or misshapen, as if galaxies of similar size are colliding. Even the calmer-looking galaxies are often clumpy and irregular. Instead of having smooth disks or spiral arms, early galaxies are d ...
... But at cosmic high noon, when stars were blazing into existence at peak rates, many galaxies look distorted or misshapen, as if galaxies of similar size are colliding. Even the calmer-looking galaxies are often clumpy and irregular. Instead of having smooth disks or spiral arms, early galaxies are d ...
The Hipparcos Star Globe Booklet - Cosmos
... Galaxy with positions, distances and velocities of stars. Significantly, Gaia’s observing programme will be complete and unbiased, thereby producing a representative sample of the Galactic population, whilst Hipparcos based its observations on a pre-selected set of bright stars. Hipparcos brought hu ...
... Galaxy with positions, distances and velocities of stars. Significantly, Gaia’s observing programme will be complete and unbiased, thereby producing a representative sample of the Galactic population, whilst Hipparcos based its observations on a pre-selected set of bright stars. Hipparcos brought hu ...
Using photometric analysis to determine characteristics of the V
... after the scientist who discovered it) whereby the pressure at the center will exceed the threshold for the carbon and oxygen nuclei to start to fuse uncontrollably [2]. This phenomenon results in a thermonuclear detonation of the star which explains the sudden increase in optical ...
... after the scientist who discovered it) whereby the pressure at the center will exceed the threshold for the carbon and oxygen nuclei to start to fuse uncontrollably [2]. This phenomenon results in a thermonuclear detonation of the star which explains the sudden increase in optical ...
The 2006 RBSE Journal - National Optical Astronomy Observatory
... To pick a target I went to http://gtn.sonoma.edu/participants/catalog and looked the objects listed. I decided to use the target AO 0235+164, an AGN, for my project. I used Starry Night Pro 3.1 to locate and predict where the target would be for observation. After imputing the Right Ascension (RA) a ...
... To pick a target I went to http://gtn.sonoma.edu/participants/catalog and looked the objects listed. I decided to use the target AO 0235+164, an AGN, for my project. I used Starry Night Pro 3.1 to locate and predict where the target would be for observation. After imputing the Right Ascension (RA) a ...
Galaxy Sorting
... types of galaxies, differences that were not known when Hubble first classified them. Elliptical galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to mak ...
... types of galaxies, differences that were not known when Hubble first classified them. Elliptical galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to mak ...
A Stars
... • B Stars (15-30,000 K): Most of H is ionized, so only very weak H lines. • A Stars (10,000 K): Ideal excitation conditions, strongest H lines. • G Stars (6000 K): Too cool, little excited H, so only weak H lines. ...
... • B Stars (15-30,000 K): Most of H is ionized, so only very weak H lines. • A Stars (10,000 K): Ideal excitation conditions, strongest H lines. • G Stars (6000 K): Too cool, little excited H, so only weak H lines. ...
Distance
... • (a) If necessary, add corrections for [Fe/H] differences to ZAMS and isochrones family, constructed for solar metallicity • (b) Match observed cluster CMD (colormagnitude diagram) to ZAMS and isochrone trying to fit cluster turn-off point • (c) Calculate horizontal and vertical offsets: ...
... • (a) If necessary, add corrections for [Fe/H] differences to ZAMS and isochrones family, constructed for solar metallicity • (b) Match observed cluster CMD (colormagnitude diagram) to ZAMS and isochrone trying to fit cluster turn-off point • (c) Calculate horizontal and vertical offsets: ...
Слайд 1 - Tuorla Observatory
... • (a) If necessary, add corrections for [Fe/H] differences to ZAMS and isochrones family, constructed for solar metallicity • (b) Match observed cluster CMD (colormagnitude diagram) to ZAMS and isochrone trying to fit cluster turn-off point • (c) Calculate horizontal and vertical offsets: ...
... • (a) If necessary, add corrections for [Fe/H] differences to ZAMS and isochrones family, constructed for solar metallicity • (b) Match observed cluster CMD (colormagnitude diagram) to ZAMS and isochrone trying to fit cluster turn-off point • (c) Calculate horizontal and vertical offsets: ...
star
... • The hottest stars, with surface temperatures above 30,000 K, appear blue. • The surfaces (photospheres) of relatively cool red stars are still a toasty 3000 K or so. • Stars with surface temperatures between 5000 and 6000 K appear yellow, like the sun. ...
... • The hottest stars, with surface temperatures above 30,000 K, appear blue. • The surfaces (photospheres) of relatively cool red stars are still a toasty 3000 K or so. • Stars with surface temperatures between 5000 and 6000 K appear yellow, like the sun. ...
ACTIVE GALAXIES
... • STARBURST galaxies -- 100's of stars forming per year, but spread over some 100's of parsecs. • Other PECULIAR galaxies involve collisions or mergers between galaxies. • Sometimes produce strong spiral structure (e.g. M51, the "Whirlpool") • Sometimes leave long tidal tails (e.g. the "Antennae" ga ...
... • STARBURST galaxies -- 100's of stars forming per year, but spread over some 100's of parsecs. • Other PECULIAR galaxies involve collisions or mergers between galaxies. • Sometimes produce strong spiral structure (e.g. M51, the "Whirlpool") • Sometimes leave long tidal tails (e.g. the "Antennae" ga ...
Here - Astrophysics Research Institute
... Unfortunately no coordinate system can be permanently fixed. This is because the Earth's rotation axis precesses slowly, with a period of 25,600 years. This happens because the Earth is not quite spherical, but is oblate and tilted. Therefore, the direction of the Sun's gravity does not pass directl ...
... Unfortunately no coordinate system can be permanently fixed. This is because the Earth's rotation axis precesses slowly, with a period of 25,600 years. This happens because the Earth is not quite spherical, but is oblate and tilted. Therefore, the direction of the Sun's gravity does not pass directl ...
Gaps
... Recio-Blanco et al., ApJL 572, 2002 • Fast HB rotation, although maybe not present in all clusters, is a fairly common feature. ...
... Recio-Blanco et al., ApJL 572, 2002 • Fast HB rotation, although maybe not present in all clusters, is a fairly common feature. ...
Aries (constellation)
Aries is one of the constellations of the zodiac. It is located in the northern celestial hemisphere between Pisces to the west and Taurus to the east. The name Aries is Latin for ram, and its symbol is 20px (Unicode ♈), representing a ram's horns. It is one of the 48 constellations described by the 2nd century astronomer Ptolemy, and remains one of the 88 modern constellations. It is a mid-sized constellation, ranking 39th overall size, with an area of 441 square degrees (1.1% of the celestial sphere).Although Aries came to represent specifically the ram whose fleece became the Golden Fleece of Ancient Greek mythology, it has represented a ram since late Babylonian times. Before that, the stars of Aries formed a farmhand. Different cultures have incorporated the stars of Aries into different constellations including twin inspectors in China and a porpoise in the Marshall Islands. Aries is a relatively dim constellation, possessing only four bright stars: Hamal (Alpha Arietis, second magnitude), Sheratan (Beta Arietis, third magnitude), Mesarthim (Gamma Arietis, fourth magnitude), and 41 Arietis (also fourth magnitude). The few deep-sky objects within the constellation are quite faint and include several pairs of interacting galaxies. Several meteor showers appear to radiate from Aries, including the Daytime Arietids and the Epsilon Arietids.