High-mass star-forming cloud G0.38+0.04 in the Galactic center dust
... >20 are not possible, so additional physical mechanisms must be in play for the brightest H2 CO masers. SiO masers are common toward oxygen-rich evolved stars, namely long period variables (Mira stars) and red supergiants ...
... >20 are not possible, so additional physical mechanisms must be in play for the brightest H2 CO masers. SiO masers are common toward oxygen-rich evolved stars, namely long period variables (Mira stars) and red supergiants ...
Observational evidence for AGN feedback in early
... activity, black hole activity, the composite of the two and quiescence. We find that emission is mostly LINER (low ionization nuclear emission line region) like in high-mass galaxies (σ > 200 km s−1 ) and roughly evenly distributed between star formation and AGN at intermediate and low (σ < 100 km s ...
... activity, black hole activity, the composite of the two and quiescence. We find that emission is mostly LINER (low ionization nuclear emission line region) like in high-mass galaxies (σ > 200 km s−1 ) and roughly evenly distributed between star formation and AGN at intermediate and low (σ < 100 km s ...
Galaxies
... SDSS or 2MASS, and are also difficult targets for spectroscopy. Our census of the local Universe is highly incomplete for such galaxies. Figure 9.6 shows some typical example morphologies. Figure 9.7 shows the magnitude–radius relation for dwarf galaxies at a variety of distances. Nearby dwarf galax ...
... SDSS or 2MASS, and are also difficult targets for spectroscopy. Our census of the local Universe is highly incomplete for such galaxies. Figure 9.6 shows some typical example morphologies. Figure 9.7 shows the magnitude–radius relation for dwarf galaxies at a variety of distances. Nearby dwarf galax ...
A Universal Stellar Initial Mass Function? A Critical Look Further
... The last observational problem for determining the IMF that we address is stellar (and substellar) multiplicity. Many stellar objects are found to have gravitationally bound companions of lower mass (by conventional definition) and at a variety of orbital separations. If we consider that many determ ...
... The last observational problem for determining the IMF that we address is stellar (and substellar) multiplicity. Many stellar objects are found to have gravitationally bound companions of lower mass (by conventional definition) and at a variety of orbital separations. If we consider that many determ ...
The properties of a spectroscopically selected sample of cataclysmic variables Amornrat Aungwerojwit
... I would like to thank Dr. Boris G¨ansicke for being a superb supervisor in guiding me during my PhD. Without his useful suggestions, constructive comments, kindness, and patience, the work presented in this thesis could not have been satisfactory. I am grateful for his enthusiasm, which has inspired ...
... I would like to thank Dr. Boris G¨ansicke for being a superb supervisor in guiding me during my PhD. Without his useful suggestions, constructive comments, kindness, and patience, the work presented in this thesis could not have been satisfactory. I am grateful for his enthusiasm, which has inspired ...
Isaac NEWTON: Philosophiae Naturalis Principia Mathematica. 3 Ed
... 30 or 4 to 5. Again the comet of the year 1665 in the month of April, as Helvelius is the authority, by its clarity surpassed almost all the fixed stars, even Saturn, on account of the vividness of its colour for a long while. Certainly this comet was brighter than that other one, which had appeared ...
... 30 or 4 to 5. Again the comet of the year 1665 in the month of April, as Helvelius is the authority, by its clarity surpassed almost all the fixed stars, even Saturn, on account of the vividness of its colour for a long while. Certainly this comet was brighter than that other one, which had appeared ...
Worlds Beyond: A Strategy for the Detection and Characterization of
... fitting formulas of Fortney et al. (2007) (specifically, loge was used instead of log10 ). Fig. 1 shows the original and corrected mass-radius relations. The most important effect of this error was to make the prospects for using JWST/NIRSpec to characterize the atmospheres of transiting planets app ...
... fitting formulas of Fortney et al. (2007) (specifically, loge was used instead of log10 ). Fig. 1 shows the original and corrected mass-radius relations. The most important effect of this error was to make the prospects for using JWST/NIRSpec to characterize the atmospheres of transiting planets app ...
Chapter 5 The Evolutionary Paths Of Nearby Galaxies
... increasing the stellar mass retained in quiescent systems. In this case, a quenching of the star formation is required to drive galaxies towards the red sequence, but it is still unclear what physical mechanism(s) may be responsible for such migration. The most popular candidate is feedback from the ...
... increasing the stellar mass retained in quiescent systems. In this case, a quenching of the star formation is required to drive galaxies towards the red sequence, but it is still unclear what physical mechanism(s) may be responsible for such migration. The most popular candidate is feedback from the ...
Jul y 10-12,
... IGR J17091-3624 is a black hole system which has very recently attracted the interest in the scientific community as it is the first system to show some of the bizarre, high-amplitude, highly-structured X-ray variability only seen before in the extremely energetic black hole system GRS 1915+105. In ...
... IGR J17091-3624 is a black hole system which has very recently attracted the interest in the scientific community as it is the first system to show some of the bizarre, high-amplitude, highly-structured X-ray variability only seen before in the extremely energetic black hole system GRS 1915+105. In ...
The physics of line-driven winds of hot massive stars
... Their luminosities can be more than a million times that of our Sun, which is considered a nominal star. These stars are also the most massive ones, some of them starting their lives with perhaps more than a hundred times the mass of our Sun. Although spectacular objects, massive stars are rare. Dep ...
... Their luminosities can be more than a million times that of our Sun, which is considered a nominal star. These stars are also the most massive ones, some of them starting their lives with perhaps more than a hundred times the mass of our Sun. Although spectacular objects, massive stars are rare. Dep ...
Differential rotation in Sun-like stars from surface variability and
... to play a key role in the generation of magnetic fields. So far however, the internal rotation profiles of stars other than the Sun are unknown, and placing constraints on models of rotation and magnetic dynamos is therefore difficult. The NASA Kepler mission has provided high-quality photometric da ...
... to play a key role in the generation of magnetic fields. So far however, the internal rotation profiles of stars other than the Sun are unknown, and placing constraints on models of rotation and magnetic dynamos is therefore difficult. The NASA Kepler mission has provided high-quality photometric da ...
Multiplicity in Early Stellar Evolution - Astronomy Group
... systems of two or more bodies is the norm at all stellar evolutionary stages. Multiple systems are widely agreed to result from the collapse and fragmentation of cloud cores, despite the inhibiting influence of magnetic fields. Surveys of class 0 protostars with millimeter interferometers have revea ...
... systems of two or more bodies is the norm at all stellar evolutionary stages. Multiple systems are widely agreed to result from the collapse and fragmentation of cloud cores, despite the inhibiting influence of magnetic fields. Surveys of class 0 protostars with millimeter interferometers have revea ...
Gamma-Ray Bursts and Puzzles of Core
... results of the photometric measurement of z applied to galaxies from the Hubble Deep Field (HDF) by Fernández et al. (1999). Circles denote the GRB host galaxies with the BTA photometry, asterisks are results by other authors (HST, VLT). For the galaxy GRB 991208 first measurement of z = 0.706 and R ...
... results of the photometric measurement of z applied to galaxies from the Hubble Deep Field (HDF) by Fernández et al. (1999). Circles denote the GRB host galaxies with the BTA photometry, asterisks are results by other authors (HST, VLT). For the galaxy GRB 991208 first measurement of z = 0.706 and R ...
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.