Rotation Periods of Wide Binaries in the Kepler Field
... Because most of the stars that satisfy the present criteria are relatively nearby, they should be expected to have low interstellar reddening. In any case, since the two components presumably lie at the same distance, the reddening would be expected to be the same, and so will not affect Figure 1. T ...
... Because most of the stars that satisfy the present criteria are relatively nearby, they should be expected to have low interstellar reddening. In any case, since the two components presumably lie at the same distance, the reddening would be expected to be the same, and so will not affect Figure 1. T ...
Chapter 15 THE MILKY WAY IN RELATION TO OTHER GALAXIES
... radially exponential surface brightness distribution; most bars in spiral galaxies however, have a fairly constant surface brightness. At 2◦.8 a faster decline than the exponential sets in in all colors and this may indicate the onset of a truncation of the stellar distribution caused by the tidal f ...
... radially exponential surface brightness distribution; most bars in spiral galaxies however, have a fairly constant surface brightness. At 2◦.8 a faster decline than the exponential sets in in all colors and this may indicate the onset of a truncation of the stellar distribution caused by the tidal f ...
Chemical abundances and winds of massive stars in M31: a Btype
... morphology of their UV spectra compared to OB 10-64. These two stars have essentially little or no internal Large Magellanic Cloud (LMC) extinction and the EðB 2 VÞ values (0.06 and 0.10 respectively) reflect the reddening from intervening Galactic material. This Milky Way extinction is similar to w ...
... morphology of their UV spectra compared to OB 10-64. These two stars have essentially little or no internal Large Magellanic Cloud (LMC) extinction and the EðB 2 VÞ values (0.06 and 0.10 respectively) reflect the reddening from intervening Galactic material. This Milky Way extinction is similar to w ...
Chapter 1 The Discovery of Open Clusters - Willmann-Bell
... morphological features he found in the nebulae and clusters that he discovered. In this he used the evidence of his extensive star count surveys, or gauges. Having gauged the Milky Way in various places, he concluded that the number of stars “constantly increase and decrease in proportion to its app ...
... morphological features he found in the nebulae and clusters that he discovered. In this he used the evidence of his extensive star count surveys, or gauges. Having gauged the Milky Way in various places, he concluded that the number of stars “constantly increase and decrease in proportion to its app ...
PPT presentation
... first 2.5 mags of its PNLF. Steep turnover at high L’s interpreted as due to sharp cutoff to upper mass limit of PN central stars. ...
... first 2.5 mags of its PNLF. Steep turnover at high L’s interpreted as due to sharp cutoff to upper mass limit of PN central stars. ...
Processing of Star Catalog and Star Image
... 6 × 9 × 9 = 486 sub-blocks and then the direction vector of each sub-block’s corresponding central axis can be obtained. 486 boresight pointings (direction vector) evenly distributed in the full sky resulting from this method and the angle between each pair of neighboring boresight pointings is 10°. ...
... 6 × 9 × 9 = 486 sub-blocks and then the direction vector of each sub-block’s corresponding central axis can be obtained. 486 boresight pointings (direction vector) evenly distributed in the full sky resulting from this method and the angle between each pair of neighboring boresight pointings is 10°. ...
A Detailed Derivation of the Radial Velocity Equation
... Now we need to set up a coordinate system (shown in Figure 2) and review some basics of vectors. 4 THE RADIAL VELOCITY EQUATION ...
... Now we need to set up a coordinate system (shown in Figure 2) and review some basics of vectors. 4 THE RADIAL VELOCITY EQUATION ...
The Deaths of Very Massive Stars
... relativity in three dimensions, the existence of stellar mass black holes and the absence of observable supernova progenitors with high mass implies that at least some stars do not explode and eject all of their heavy element inventory. Until such time as credible models exist, a reasonable assumpti ...
... relativity in three dimensions, the existence of stellar mass black holes and the absence of observable supernova progenitors with high mass implies that at least some stars do not explode and eject all of their heavy element inventory. Until such time as credible models exist, a reasonable assumpti ...
The Classification of Stellar Spectra
... Background: The History And Nature Of Spectral Classification Patterns of absorption lines were first observed in the spectrum of the sun by the German physicist Joseph von Fraunhofer early in the 1800’s, but it was not until late in the century that astronomers were able to routinely examine the sp ...
... Background: The History And Nature Of Spectral Classification Patterns of absorption lines were first observed in the spectrum of the sun by the German physicist Joseph von Fraunhofer early in the 1800’s, but it was not until late in the century that astronomers were able to routinely examine the sp ...
Measurements of Neutron Star Masses
... 2 This way, TEMPO settles 2 on a DM 1 for 2this any given epoch. day that produces the best overall fit. This can bring to light intrinsic DM variations, but it can also absorb other frequency dependent effects. On two days, outliers suggest instrument 1 Figs. 9 and 10), and these problems (MJDs 535 ...
... 2 This way, TEMPO settles 2 on a DM 1 for 2this any given epoch. day that produces the best overall fit. This can bring to light intrinsic DM variations, but it can also absorb other frequency dependent effects. On two days, outliers suggest instrument 1 Figs. 9 and 10), and these problems (MJDs 535 ...
Stars & Galaxies - newmanlib.ibri.org
... that they differ in brightness. • As one looks at the stars more carefully, it becomes apparent that they are not all the same color. • Look at the constellation of Orion shown in the next panel. ...
... that they differ in brightness. • As one looks at the stars more carefully, it becomes apparent that they are not all the same color. • Look at the constellation of Orion shown in the next panel. ...
a wide-field survey for variable stars
... The orange star at the center of the image is T Tauri, prototype of the class of T Tauri variable stars. The nearby dusty, yellow cloud is Hind’s Variable Nebula (NGC 1555/1554). Over 400 light-years away, at the edge of a molecular cloud, both star and nebula are seen to vary significantly in brigh ...
... The orange star at the center of the image is T Tauri, prototype of the class of T Tauri variable stars. The nearby dusty, yellow cloud is Hind’s Variable Nebula (NGC 1555/1554). Over 400 light-years away, at the edge of a molecular cloud, both star and nebula are seen to vary significantly in brigh ...
Stargazing For Beginners: A Binocular Tour of the Southern Night Sky
... angular distances using nothing more than your hands and fingers held at arm’s length. While simple, this is an essential skill for finding your way around the night sky. The sky tours cover four three-month seasons starting from June through August, which marks the late Autumn and winter in the sou ...
... angular distances using nothing more than your hands and fingers held at arm’s length. While simple, this is an essential skill for finding your way around the night sky. The sky tours cover four three-month seasons starting from June through August, which marks the late Autumn and winter in the sou ...
Article PDF - IOPscience
... moderately metal-poor ([Fe/H] ∼ −1.3 dex), while Oo II clusters were very metal-poor ([Fe/H] ∼ −2.0 dex). Recent studies (see, e.g., Catelan 2009, for a review) involving larger samples of GCs, more accurate metallicities, better periods for the RRL stars, and higher completeness, have fully confirm ...
... moderately metal-poor ([Fe/H] ∼ −1.3 dex), while Oo II clusters were very metal-poor ([Fe/H] ∼ −2.0 dex). Recent studies (see, e.g., Catelan 2009, for a review) involving larger samples of GCs, more accurate metallicities, better periods for the RRL stars, and higher completeness, have fully confirm ...
Colloquial Jakartan Indonesian
... record their navigational strategies. His resulting book, We, the Navigators (1972),2 is the most complete record we are likely to get of this body of knowledge, rapidly disappearing with the increased presence of motorised boats and Western navigational technology. He was also at pains to record, i ...
... record their navigational strategies. His resulting book, We, the Navigators (1972),2 is the most complete record we are likely to get of this body of knowledge, rapidly disappearing with the increased presence of motorised boats and Western navigational technology. He was also at pains to record, i ...
The accretion disk paradigm for young stars
... whereas the observed excess luminosity can be greater than L in extreme CTTSs. Even though the value of a typical CTTS luminosity excess was unknown in the early 1950s, it was already clear that it was orders of magnitude larger than what the accretion of interstellar cloud gas could provide. Faced ...
... whereas the observed excess luminosity can be greater than L in extreme CTTSs. Even though the value of a typical CTTS luminosity excess was unknown in the early 1950s, it was already clear that it was orders of magnitude larger than what the accretion of interstellar cloud gas could provide. Faced ...
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... from Ita et al. (1994). For stars classified as Miras we used Ita’s relation C including their separation for targets with J − K < 1.4 and J − K > 1.4. For semi-regular variables we used sequence B or C’. Naturally, this approach includes some uncertainties. In their Table 3, Ita et al. (1994) list ...
... from Ita et al. (1994). For stars classified as Miras we used Ita’s relation C including their separation for targets with J − K < 1.4 and J − K > 1.4. For semi-regular variables we used sequence B or C’. Naturally, this approach includes some uncertainties. In their Table 3, Ita et al. (1994) list ...
SherwoodWA_1973redux - Edinburgh Research Archive
... 1970; Gottesman and Davis, 1970) found that the HII regions and blue supergiants (in associations) lie within the ...
... 1970; Gottesman and Davis, 1970) found that the HII regions and blue supergiants (in associations) lie within the ...
January 2014 Astronomy Calendar by Dave Mitsky Some
... extreme crescent Moons. Times and dates for the lunar light rays predicted to occur this month are available at http://www.lunar-occultations.com/rlo/rays/rays.htm The Sun is located in Sagittarius on January 1st. Data (magnitude, apparent size, illumination, and distance from the Earth in astronomi ...
... extreme crescent Moons. Times and dates for the lunar light rays predicted to occur this month are available at http://www.lunar-occultations.com/rlo/rays/rays.htm The Sun is located in Sagittarius on January 1st. Data (magnitude, apparent size, illumination, and distance from the Earth in astronomi ...
Comparing stars - The Open University
... Above and to the left of the red giants we come to the supergiants. These are larger, and thus more luminous than red giants of comparable temperature, but they also extend to higher temperatures, where they are larger and more luminous than main sequence stars of comparable temperature. Rigel A is ...
... Above and to the left of the red giants we come to the supergiants. These are larger, and thus more luminous than red giants of comparable temperature, but they also extend to higher temperatures, where they are larger and more luminous than main sequence stars of comparable temperature. Rigel A is ...
1 CHAPTER 18 SPECTROSCOPIC BINARY STARS 18.1
... distinguish the two components even with a large telescope – but we can detect the fact that there are two stars from their spectra. In favourable circumstances, two distinct spectra can be seen. It might be that the spectral types of the two components are very different – perhaps a hot A-type star ...
... distinguish the two components even with a large telescope – but we can detect the fact that there are two stars from their spectra. In favourable circumstances, two distinct spectra can be seen. It might be that the spectral types of the two components are very different – perhaps a hot A-type star ...
Boötes
Boötes /boʊˈoʊtiːz/ is a constellation in the northern sky, located between 0° and +60° declination, and 13 and 16 hours of right ascension on the celestial sphere. The name comes from the Greek Βοώτης, Boōtēs, meaning herdsman or plowman (literally, ox-driver; from βοῦς bous “cow”). The ""ö"" in the name is a diaeresis, not an umlaut, meaning that each 'o' is to be pronounced separately.One of the 48 constellations described by the 2nd century astronomer Ptolemy, Boötes is now one of the 88 modern constellations. It contains the fourth brightest star in the night sky, the orange-hued Arcturus. Boötes is home to many other bright stars, including eight above the fourth magnitude and an additional 21 above the fifth magnitude, making a total of 29 stars easily visible to the naked eye.