Galaxies
... • Astronomers now have decided that the morphology classification should consist of only two types of galaxies: the spiral and the elliptical. • Barred spirals are a subclass of spirals. Irregulars may be either spiral or barred spiral. ...
... • Astronomers now have decided that the morphology classification should consist of only two types of galaxies: the spiral and the elliptical. • Barred spirals are a subclass of spirals. Irregulars may be either spiral or barred spiral. ...
A scenario of planet erosion by coronal radiation*
... magnitude in the LX levels of stars of the same spectral type and age (Penz et al. 2008; Penz & Micela 2008). The accumulated X-ray flux at the planet orbit is shown in Fig. 2. Subgiants are marked with different symbols since it is not known whether they follow the same relation. A hard limit of ∼10 ...
... magnitude in the LX levels of stars of the same spectral type and age (Penz et al. 2008; Penz & Micela 2008). The accumulated X-ray flux at the planet orbit is shown in Fig. 2. Subgiants are marked with different symbols since it is not known whether they follow the same relation. A hard limit of ∼10 ...
Mode Identification
... ▸ Theoretical amplitude ratios and phase differences depend on the stellar flux. ▸ The stellar flux is determined by the metallicity, the effective temperature, the mass and the radius, or equivalently, by the gravity, of the star. ▸ Parameters are often not well known; their errors propagate into t ...
... ▸ Theoretical amplitude ratios and phase differences depend on the stellar flux. ▸ The stellar flux is determined by the metallicity, the effective temperature, the mass and the radius, or equivalently, by the gravity, of the star. ▸ Parameters are often not well known; their errors propagate into t ...
Observing binaries with Gaia
... • Millions of binaries of all kinds • Complete statistics near sun • Partial statistics over large parts of the Galaxy • Orbits and masses ...
... • Millions of binaries of all kinds • Complete statistics near sun • Partial statistics over large parts of the Galaxy • Orbits and masses ...
Dynamical Interactions Make Hot Jupiters in Open Star Clusters
... this paper is that three of the inner Jupiters reach a = 0.33 AU (e = 0.985), a = 0.035 AU (e = 0.616), and a = 0.012 AU (e = 0.2) respectively, from their host stars, as detailed below. We emphasize that the formation of these three hot Jupiters is driven by passages of cluster stars near the plane ...
... this paper is that three of the inner Jupiters reach a = 0.33 AU (e = 0.985), a = 0.035 AU (e = 0.616), and a = 0.012 AU (e = 0.2) respectively, from their host stars, as detailed below. We emphasize that the formation of these three hot Jupiters is driven by passages of cluster stars near the plane ...
12-iim fine-structure emission line and continuum images of G333.6
... Aitken & Jones (1974). They interpreted the almost featureless spectrum (i.e. lacking the typical 10-Rm silicate feature) as re-absorption of thermal emission from optically thin dust containing silicates, by a cooler envelope of similar material surrounding the hotter emitting core. From these obse ...
... Aitken & Jones (1974). They interpreted the almost featureless spectrum (i.e. lacking the typical 10-Rm silicate feature) as re-absorption of thermal emission from optically thin dust containing silicates, by a cooler envelope of similar material surrounding the hotter emitting core. From these obse ...
classifying stars
... (HOW BRIGHT A STAR APPEARS.) However, if astronomers could take two stars and place them exactly the same distance from earth, they could tell which one really is brighter... unfortunately, this is not possible, but astronomers can measure the amount of light a star actually gives off. This is calle ...
... (HOW BRIGHT A STAR APPEARS.) However, if astronomers could take two stars and place them exactly the same distance from earth, they could tell which one really is brighter... unfortunately, this is not possible, but astronomers can measure the amount of light a star actually gives off. This is calle ...
talk
... Substantial fine scale structure visible at high resolution Scales of energy injection into ISM through stellar winds/supernovae ...
... Substantial fine scale structure visible at high resolution Scales of energy injection into ISM through stellar winds/supernovae ...
A cold detached dust envelope around an oxygen-rich Mira
... and 100 µm images of R Hya are shown in Fig. 2a and b, respectively. The 60 µm image (Fig. 2a) shows a definite component of the extended emission around R Hya with an effective spatial resolution about 1 arc minute. The extended component is also seen in the 100 µm image (Fig. 2b), though detailed ...
... and 100 µm images of R Hya are shown in Fig. 2a and b, respectively. The 60 µm image (Fig. 2a) shows a definite component of the extended emission around R Hya with an effective spatial resolution about 1 arc minute. The extended component is also seen in the 100 µm image (Fig. 2b), though detailed ...
Spectral modeling of nebular-phase supernovae Anders Jerkstrand Department of Astronomy
... Massive stars live fast and die young. They shine furiously for a few million years, during which time they synthesize most of the heavy elements in the universe in their cores. They end by blowing themselves up in a powerful explosion known as a supernova (SN). During this process, the core collaps ...
... Massive stars live fast and die young. They shine furiously for a few million years, during which time they synthesize most of the heavy elements in the universe in their cores. They end by blowing themselves up in a powerful explosion known as a supernova (SN). During this process, the core collaps ...
Evolution of stars
... e. they are all so far away that the light hasn't reached us yet. The nuclear reactions in a star's core remain under control so long as a. luminosity depends on mass. b. pressure depends on temperature. c. density depends on mass. d. weight depends on temperature. e. temperature depends on mass. In ...
... e. they are all so far away that the light hasn't reached us yet. The nuclear reactions in a star's core remain under control so long as a. luminosity depends on mass. b. pressure depends on temperature. c. density depends on mass. d. weight depends on temperature. e. temperature depends on mass. In ...
Isotopic composition of Hg and Pt in 5 slowly rotating HgMn stars *
... 1:67 for the ratio of the radii of the primary to the secondary stars, and Te = 9200 K, log g = 4:2, a microturbulent velocity = 2:0 km s;1 , and v sin i = 2 km s;1 for the secondary. Furthermore, we assumed solar chemical composition for this star, in spite of the fact that Wahlgren at al. (1994 ...
... 1:67 for the ratio of the radii of the primary to the secondary stars, and Te = 9200 K, log g = 4:2, a microturbulent velocity = 2:0 km s;1 , and v sin i = 2 km s;1 for the secondary. Furthermore, we assumed solar chemical composition for this star, in spite of the fact that Wahlgren at al. (1994 ...
VISIBLE STARS AS APPARENT OBSERVATIONAL EVIDENCE IN
... 5 Graney (2007) concludes that the linear relationship between α and M implied in the Dialogue is consistent with what would be seen through the telescope, which could suggest that Galileo's 5/6” diameter for 6th magnitude stars is a projection from a trend. Graney page 16 ...
... 5 Graney (2007) concludes that the linear relationship between α and M implied in the Dialogue is consistent with what would be seen through the telescope, which could suggest that Galileo's 5/6” diameter for 6th magnitude stars is a projection from a trend. Graney page 16 ...
Facilitator`s Guide
... Introduction: People young and old have always been fascinated and awed by imagining how large and how old the Universe is and how far away the stars and the galaxies are from us. Today, many simply accept these huge numbers they hear as fact, without wondering how they are ascertained. In a typical ...
... Introduction: People young and old have always been fascinated and awed by imagining how large and how old the Universe is and how far away the stars and the galaxies are from us. Today, many simply accept these huge numbers they hear as fact, without wondering how they are ascertained. In a typical ...
1. INTRODUCTION 2. THE MODEL
... C. Hayashi prescribed a ““ minimum-mass solar nebula,ÏÏ which contained just enough material to make the planets. This prescription, which has been widely used in constructing scenarios for planet formation, proposed that ice will condense when the temperature falls below 170 K (the ““ snow line ÏÏ) ...
... C. Hayashi prescribed a ““ minimum-mass solar nebula,ÏÏ which contained just enough material to make the planets. This prescription, which has been widely used in constructing scenarios for planet formation, proposed that ice will condense when the temperature falls below 170 K (the ““ snow line ÏÏ) ...
Chapter13- Star Stuff-pptx - SFA Physics and Astronomy
... What have we learned? • What are the life stages of a high-mass star? – They are similar to the life stages of a low-mass star. • How do high-mass stars make the elements necessary for life? – Higher masses produce higher core temperatures that enable fusion of heavier elements. • How does a high-m ...
... What have we learned? • What are the life stages of a high-mass star? – They are similar to the life stages of a low-mass star. • How do high-mass stars make the elements necessary for life? – Higher masses produce higher core temperatures that enable fusion of heavier elements. • How does a high-m ...
Measuring Astronomical Distances
... Cepheid Variables - http://hyperphysics.phy-astr.gsu.edu/hbase/astro/cepheid.html ...
... Cepheid Variables - http://hyperphysics.phy-astr.gsu.edu/hbase/astro/cepheid.html ...
... HST imaging of 10 compact PNe (Hsia et al. 2014) shows that multipolar structures are common, indicating multiple phases of ejection and shaping. The paper does not state how the target sample was selected, so that rates of occurence cannot be inferred. A new member of the small class of PNe with ex ...
Galaxy Evolution
... The Great Wall of Galaxies The largest structure yet found in the Universe 280 x 700 million light years in size less than 20 million light years thick diagonally across the northern sky similar structure across the southern sky are they related? ...
... The Great Wall of Galaxies The largest structure yet found in the Universe 280 x 700 million light years in size less than 20 million light years thick diagonally across the northern sky similar structure across the southern sky are they related? ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.