Module1: Scale of the Universe
... Ask&your&students&to&discuss&some&possible&difBiculties&of&measuring&cosmic& distances&using¶llax.&Ensure&they&mention&the&following&points:& Parallax&shifts&are&always&small.&& Parallax&shift&is&even&smaller&than&the&apparent&size&of&the&star.&In&additional,& starlight&is&refracted&by&Earth's&a ...
... Ask&your&students&to&discuss&some&possible&difBiculties&of&measuring&cosmic& distances&using¶llax.&Ensure&they&mention&the&following&points:& Parallax&shifts&are&always&small.&& Parallax&shift&is&even&smaller&than&the&apparent&size&of&the&star.&In&additional,& starlight&is&refracted&by&Earth's&a ...
Evolution of stars
... c. can not be used to estimate the luminosity of the star. d. are very weak and difficult to see. e. are useful in determining the apparent magnitude of the star. 2. Parallax would be easier to measure if a. Earth's orbit were larger. b. the stars were farther away. c. Earth moved faster along its o ...
... c. can not be used to estimate the luminosity of the star. d. are very weak and difficult to see. e. are useful in determining the apparent magnitude of the star. 2. Parallax would be easier to measure if a. Earth's orbit were larger. b. the stars were farther away. c. Earth moved faster along its o ...
astro-ph/0303282 PDF
... equal to the proper motion of the primary star; in fact, within the errors, no candidates changed their relative positions. Vega source 7 changed position at the 3 sigma level, but not in the direction expected for a true companion. This source is located near the edge of the image and may be subjec ...
... equal to the proper motion of the primary star; in fact, within the errors, no candidates changed their relative positions. Vega source 7 changed position at the 3 sigma level, but not in the direction expected for a true companion. This source is located near the edge of the image and may be subjec ...
View the sky`s greatest nebula
... Our earthbound view is rather different. On a clear summer night in the Northern Hemisphere, the glow of the Milky Way stretches from Cassiopeia in the northeast to Scorpius in the south. From this vantage point, we’re looking along the galaxy’s rim. Toward Scorpius is the central part of the Milky ...
... Our earthbound view is rather different. On a clear summer night in the Northern Hemisphere, the glow of the Milky Way stretches from Cassiopeia in the northeast to Scorpius in the south. From this vantage point, we’re looking along the galaxy’s rim. Toward Scorpius is the central part of the Milky ...
THE N/O RATIO IN EARLY B-TYPE MAIN SEQUENCE STARS AS
... logC , logN , and logO for MS B-stars found in Ref. 14, together with recent estimates of the abundances of C, N, and O for the sun [15,16]. The latter were obtained using nonstationary hydrodynamic 3D models of the solar atmosphere. We note that the elemental abundances here and in the ...
... logC , logN , and logO for MS B-stars found in Ref. 14, together with recent estimates of the abundances of C, N, and O for the sun [15,16]. The latter were obtained using nonstationary hydrodynamic 3D models of the solar atmosphere. We note that the elemental abundances here and in the ...
Discovery of extremely lead-rich subdwarfs: does heavy metal signal
... causes hydrogen to diffuse upwards, a majority are extremely helium poor. Questions posed include: when does the atmosphere become chemically stratified and at what rate? The existence of several helium-rich subdwarfs suggests further questions: are there distinct subgroups of hot subdwarf, or do ho ...
... causes hydrogen to diffuse upwards, a majority are extremely helium poor. Questions posed include: when does the atmosphere become chemically stratified and at what rate? The existence of several helium-rich subdwarfs suggests further questions: are there distinct subgroups of hot subdwarf, or do ho ...
January 2014 Astronomy Calendar by Dave Mitsky Some
... The Moon is 29.0 days old and is located in Aquarius on January 1st at 0:00 UT. Two New Moons occur this month. Large tides will occur on January 1st through January 4th and on January 30th and January 31st. The Moon is at its greatest declination north of +19.5 degrees on January 13th and its grea ...
... The Moon is 29.0 days old and is located in Aquarius on January 1st at 0:00 UT. Two New Moons occur this month. Large tides will occur on January 1st through January 4th and on January 30th and January 31st. The Moon is at its greatest declination north of +19.5 degrees on January 13th and its grea ...
a changing cosmos - Whittier Union High School District
... underground crater found near Chixulub (pronounced Chi’-shooloob), Mexico, was found to be about 65 million years old. The clay layer contained tiny pieces of minerals (shocked quartz) and glassy rocks (tektites), which are found at nuclear test sites and large meteor impact sites, as well as soot—i ...
... underground crater found near Chixulub (pronounced Chi’-shooloob), Mexico, was found to be about 65 million years old. The clay layer contained tiny pieces of minerals (shocked quartz) and glassy rocks (tektites), which are found at nuclear test sites and large meteor impact sites, as well as soot—i ...
Candidate star clusters toward the inner Milky Way discovered on
... The final list of identified cluster candidates contains nine objects. Their locations on the sky are shown in Fig. 4 and there appears to be some clustering: VVV CC 169 and VVV CC 170 have projected on-sky separation of ∼2 arcmin, but these objects have different extinctions and distances (Table 1) ...
... The final list of identified cluster candidates contains nine objects. Their locations on the sky are shown in Fig. 4 and there appears to be some clustering: VVV CC 169 and VVV CC 170 have projected on-sky separation of ∼2 arcmin, but these objects have different extinctions and distances (Table 1) ...
Long-term monitoring of the short period SU UMa
... most acceptable model for SU UMa stars is the thermaltidal instability model developed by Osaki (1989), well reproducing the majority of observations. V844 Her was discovered by Antipin (1996) as a variable star near η Her. Antipin (1996) classified the variable, originally named Var 43 Her, as a dw ...
... most acceptable model for SU UMa stars is the thermaltidal instability model developed by Osaki (1989), well reproducing the majority of observations. V844 Her was discovered by Antipin (1996) as a variable star near η Her. Antipin (1996) classified the variable, originally named Var 43 Her, as a dw ...
Abundances and possible diffusion of elements in M 67 stars⋆
... vs. the means of the two photometric temperatures with the correction mentioned above. It is seen that these two temperature scales agree well. The mean difference is −2 K and the standard deviation is 46 K. There may be a tendency for the different stellar groups to behave somewhat differently, the MS ...
... vs. the means of the two photometric temperatures with the correction mentioned above. It is seen that these two temperature scales agree well. The mean difference is −2 K and the standard deviation is 46 K. There may be a tendency for the different stellar groups to behave somewhat differently, the MS ...
Planetary Nebulae: Observational Properties, Mimics, and Diagnostics
... individual PN, a large and diverse range of detection methods has been used in their discovery. Some of the brightest and best-known PNe were found over two centuries ago at the telescope eyepiece by pioneering observers like Charles Messier and William Herschel. Herschel in particular assigned nebu ...
... individual PN, a large and diverse range of detection methods has been used in their discovery. Some of the brightest and best-known PNe were found over two centuries ago at the telescope eyepiece by pioneering observers like Charles Messier and William Herschel. Herschel in particular assigned nebu ...
Comparing stars - The Open University
... (most negative apparent visual magnitude!) of any star in the night sky. This is, as we have seen, not because it is very luminous, but because it is both fairly luminous and rather close - at 2.63 pc it's the seventh closest star after the Sun. Above the lower part of the main sequence we come firs ...
... (most negative apparent visual magnitude!) of any star in the night sky. This is, as we have seen, not because it is very luminous, but because it is both fairly luminous and rather close - at 2.63 pc it's the seventh closest star after the Sun. Above the lower part of the main sequence we come firs ...
Lithium abundances along the red giant branch: FLAMES
... agreed with the expected value for the difference in heliocentric correction, and the same shift was found for all spectra obtained at a given time. Therefore, we can exclude that these shifts are the result of orbital motion in a binary system. No other velocity shifts were found within the accuracy ...
... agreed with the expected value for the difference in heliocentric correction, and the same shift was found for all spectra obtained at a given time. Therefore, we can exclude that these shifts are the result of orbital motion in a binary system. No other velocity shifts were found within the accuracy ...
Red supergiants and the past of Cygnus OB2
... stars approximately coincident with Cygnus OB2. A total of 11 sources are found within a circle of 1◦ radius centered on the association, of which 4 are non-supergiants based on existing observations. Near-infrared spectroscopy is presented of the remaining seven candidates, including four that have ...
... stars approximately coincident with Cygnus OB2. A total of 11 sources are found within a circle of 1◦ radius centered on the association, of which 4 are non-supergiants based on existing observations. Near-infrared spectroscopy is presented of the remaining seven candidates, including four that have ...
Astronomy Astrophysics First detection of the field star overdensity in the Perseus... &
... the two sets of physical parameters. This cleanest sample contains 8328 stars and is named CS-MB or CS-EC depending on whether their physical parameters were computed using the MB or EC method (see Fig. 1). This sample contains stars with more accurate SPP data, but has fewer statistics owing to the ...
... the two sets of physical parameters. This cleanest sample contains 8328 stars and is named CS-MB or CS-EC depending on whether their physical parameters were computed using the MB or EC method (see Fig. 1). This sample contains stars with more accurate SPP data, but has fewer statistics owing to the ...
The DBV stars: Progress and problems
... essentially unchanged. Other values, such as the seismological parallax also changed; the best parallax distance is now about 45 pc, and logg = 7.95. Provencal et al. (1995) find a slightly hotter temperature of 27,000 K. Depending on the carbon mass fraction in the core, I will probably be able to ...
... essentially unchanged. Other values, such as the seismological parallax also changed; the best parallax distance is now about 45 pc, and logg = 7.95. Provencal et al. (1995) find a slightly hotter temperature of 27,000 K. Depending on the carbon mass fraction in the core, I will probably be able to ...
PDF only - at www.arxiv.org.
... and the position angle = (t). The Kepler’s constant obtained is used to derive the elements of orbit. As a case study the angular separation and the position angle of the WDS 00063 +5826 and the WDS 04403-5857 were investigated. For calculating the element of orbit the Thiele-Innes van den Bos me ...
... and the position angle = (t). The Kepler’s constant obtained is used to derive the elements of orbit. As a case study the angular separation and the position angle of the WDS 00063 +5826 and the WDS 04403-5857 were investigated. For calculating the element of orbit the Thiele-Innes van den Bos me ...
Early-type stars in the core of the young open cluster Westerlund 2
... on their U BV photometry. This is also confirmed by the absence of the strong diffuse interstellar band at 4430 Å which is prominent in the spectra of the O-type members of the cluster (see Fig. 3). As we will show below, the O-stars of Westerlund 2 are subject to substantially larger reddening (AV ...
... on their U BV photometry. This is also confirmed by the absence of the strong diffuse interstellar band at 4430 Å which is prominent in the spectra of the O-type members of the cluster (see Fig. 3). As we will show below, the O-stars of Westerlund 2 are subject to substantially larger reddening (AV ...
Activity III: Calibrating Images
... by astronomers. The magnitude scale is inverse, meaning brighter stars have lower magnitudes. Absolute Magnitude - This quantity is analogous to the luminosity but is expressed on the magnitude scale. ...
... by astronomers. The magnitude scale is inverse, meaning brighter stars have lower magnitudes. Absolute Magnitude - This quantity is analogous to the luminosity but is expressed on the magnitude scale. ...
WHAT MAKES A STAR SO SPECIAL Abstract
... We know that the number of stars in the Milky Way is around 2 x 1011. Stars are not equally distributed according to their spectral class and luminosity. For every star with high luminosity from class B or O there are 350 stars from class A or K with average luminosity, or 1000 red stars from class ...
... We know that the number of stars in the Milky Way is around 2 x 1011. Stars are not equally distributed according to their spectral class and luminosity. For every star with high luminosity from class B or O there are 350 stars from class A or K with average luminosity, or 1000 red stars from class ...
Sample pages 1 PDF
... as our observations cannot penetrate the opaque core where all this interesting nuclear physics is occurring. Therefore, most AGB stars are classified as M, R, N or S, designations that have mostly been replaced by a collective term C, or “carbon stars.” Such stars have an abundance of carbon or oxyg ...
... as our observations cannot penetrate the opaque core where all this interesting nuclear physics is occurring. Therefore, most AGB stars are classified as M, R, N or S, designations that have mostly been replaced by a collective term C, or “carbon stars.” Such stars have an abundance of carbon or oxyg ...
Auriga (constellation)
Auriga is one of the 48 constellations listed by the 2nd-century astronomer Ptolemy and remains one of the 88 modern constellations. Located north of the celestial equator, its name is the Latin word for ""charioteer"", associating it with various mythological charioteers, including Erichthonius and Myrtilus. Auriga is most prominent during winter evenings in the Northern Hemisphere, along with the five other constellations that have stars in the Winter Hexagon asterism. Because of its northern declination, Auriga is only visible in its entirety as far as 34° south; for observers farther south it lies partially or fully below the horizon. A large constellation, with an area of 657 square degrees, it is half the size of the largest constellation, Hydra.Its brightest star, Capella, is an unusual multiple star system among the brightest stars in the night sky. Beta Aurigae is an interesting variable star in the constellation; Epsilon Aurigae, a nearby eclipsing binary with an unusually long period, has been studied intensively. Because of its position near the winter Milky Way, Auriga has many bright open clusters in its borders, including M36, M37, and M38, popular targets for amateur astronomers. In addition, it has one prominent nebula, the Flaming Star Nebula, associated with the variable star AE Aurigae.In Chinese mythology, Auriga's stars were incorporated into several constellations, including the celestial emperors' chariots, made up of the modern constellation's brightest stars. Auriga is home to the radiant for the Aurigids, Zeta Aurigids, Delta Aurigids, and the hypothesized Iota Aurigids.