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Chemical abundances and winds of massive stars in M31: a Btype
Chemical abundances and winds of massive stars in M31: a Btype

Orion the Hunter
Orion the Hunter

PLANETS
PLANETS

... inner edge begins around 25 AU away, farther than the average orbital distance of Uranus in the Solar System. Its outer edge appears to extend as far out as 550 AUs away from the star. Analysis of Hubble Space Telescope data indicated that planets were only beginning to form around Beta Pictoris, a ...
M13/4/PHYSI/SP3/ENG/TZ1/XX Tuesday 7 May
M13/4/PHYSI/SP3/ENG/TZ1/XX Tuesday 7 May

... On the Hertzsprung–Russell diagram, label the position of star X with the letter X. ...
Considerations about LIRIS MOS observations
Considerations about LIRIS MOS observations

... reference targets to perform mask centering. These reference targets will be located into circular apertures of 3-4” diameter and should be brighter than J=18 magnitude in order to facilitate target acquisition. Checking stars: If the brightest target (other than the reference stars) is fainter than ...
CELESTIAL COORDINATES
CELESTIAL COORDINATES

... From a latitude of 40°, an object with a declination of +40° will, at some point in time during the day or night, pass directly overhead through the zenith. In general Declination at zenith = Latitude of observer The 24 Ephemeris Stars in the SBO Catalog of Astronomical Objects have Object Numbers r ...
Condensates in Neutron Star Interiors
Condensates in Neutron Star Interiors

... On July 4th 1054, a supernova went off in the constellation of Taurus as observed widely by astronomers on Earth (and termed as nova stella, a new star). Centuries later, in 1731, John Bevis discovered the supernova remnant, which was later christened the Crab nebula (or M1, the first entry in the M ...
Rotation of KIC 11145123
Rotation of KIC 11145123

... trophysical signals with frequencies less than 0.1 d− 1 greater than 10 d). None of the pulsation frequencies in this paper are near to that lower limit, but if the star rotational signal, e.g. from starspots, that will have been he pipeline. Since, as we show, the rotation period is near y data red ...
Evolution of stars
Evolution of stars

... b. upper left corner c. upper right corner d. lower left corner e. lower right corner 6. In the H-R diagram, 90 percent of all stars are a. in the giant region. b. in the supergiant region. c. among the B stars. d. among the G stars. e. on the main sequence. 7. We know that giant stars are larger in ...
On the correlation between stellar chromospheric flux and the
On the correlation between stellar chromospheric flux and the

Document
Document

... – An H-R diagram plots the stellar luminosity of stars versus surface temperature (or color or spectral type). • What is the significance of the main sequence? – Normal stars that fuse H to He in their cores fall on the main sequence of an H-R diagram. – A star's mass determines its position along t ...
To Be or Not to Be: The Mysteries of Disk Formation Around Rapidly
To Be or Not to Be: The Mysteries of Disk Formation Around Rapidly

... • BeXRBs: ideal setting to follow disk growth and accretion fueled X-ray variations • Nearby Be disks can be resolved with the CHARA Array • Disks are smaller in K-band than in Hα • Total disk mass ranges from 8x10-8 (κ Dra) to 2x10-6 (γ Cas) solar masses • Disk filling time ≈ 1 year (BeXRBs) ...
WORD - Astrophysics
WORD - Astrophysics

Gaps
Gaps

... Recio-Blanco et al., ApJL 572, 2002 • Fast HB rotation, although maybe not present in all clusters, is a fairly common feature. ...
celestial navigation heaven`s guide for mere
celestial navigation heaven`s guide for mere

... variables. The Cepheid variables are stars that regularly pulsate in size and change in brightness. As the star increases in size, its brightness decreases; then, the reverse occurs. Cepheid variables may not be permanently variable; the fluctuations may just be an unstable phase the star is undergo ...
A Star*s Color, Temperature, and Brightness are Related!
A Star*s Color, Temperature, and Brightness are Related!

Protostellar/PMS Mass Infall Luminosity Problem
Protostellar/PMS Mass Infall Luminosity Problem

... Accretion sphere with Racc=8dx=400 AU (external accretion) ...
Magnetic fields in O-, B-and A-type stars on the main sequence
Magnetic fields in O-, B-and A-type stars on the main sequence

... time scales. For these stars with radiative envelopes, it is proven that the fields are remnants of an early phase of the star-life and one speaks of fossil fields (see Sect. 3.1.3). Over the past decade important progress has been achieved in the area of stellar magnetism. It is mainly due to the d ...
The Morning Stars
The Morning Stars

... In June 2001, NASA announced that the first Mercury orbiter mission is about to go into full-scale spacecraft development. Called ...
Direct Detection of Galactic Halo Dark Matter
Direct Detection of Galactic Halo Dark Matter

Sample
Sample

... We can measure only angular size or angular distance on the sky because we lack a simple way to measure distance to objects just by looking at them. It is therefore usually impossible to tell if we are looking at a smaller object that’s near us or a more distant object that’s much larger. Arcminutes ...
Expanding Universe and Big Bang
Expanding Universe and Big Bang

... a) The Doppler Effect is observed in sound and light. For sound, the apparent change in frequency as a source moves towards or away from a stationary observer should be investigated. The Doppler Effect causes similar shifts in wavelengths of light. The light from objects moving away from us is shift ...
How Marius Was Right and Galileo Was Wrong Even Though
How Marius Was Right and Galileo Was Wrong Even Though

The Deaths of Very Massive Stars
The Deaths of Very Massive Stars

Summary of Dynamics of the regular hendecagon: N = 11
Summary of Dynamics of the regular hendecagon: N = 11

... After 9*11 iterations of the web, H1 (and its matching segments) will yield the nine segments shown on the left above – including the crucial truncated segment that determines a side of Mx. All that we need is an ‘exact’ formula for p2, because p2 determines star[4] - since all edges must be paralle ...
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Ursa Minor



Ursa Minor (Latin: ""Smaller She-Bear"", contrasting with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the name Little Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, due to Polaris being the North Star.Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from apparent magnitude 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and magnitude 3 Gamma Ursae Minoris have been called the ""guardians of the pole star"". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered with a surface temperature of 200,000 K.
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