Hot Gas In and Around Elliptical Galaxies William G. Mathews
... galactic outflow. But in optically bright, X-ray luminous E galaxies, supernova heating is generally unable to balance the radiative losses from the hot plasma that produces the X-ray emission we observe. Paradoxically, the loss of radiative energy from the hot gas does not result in a proportional ...
... galactic outflow. But in optically bright, X-ray luminous E galaxies, supernova heating is generally unable to balance the radiative losses from the hot plasma that produces the X-ray emission we observe. Paradoxically, the loss of radiative energy from the hot gas does not result in a proportional ...
LCM Analysis for PLATO 2.0
... Summary: parameters of the system, parameters of the star spot The key to the understanding what happens on the surface of the close binary is hidden in the evolution of its light curve. The typical timescale of surface activity in short-period binaries last from several up to a few hundreds of orbi ...
... Summary: parameters of the system, parameters of the star spot The key to the understanding what happens on the surface of the close binary is hidden in the evolution of its light curve. The typical timescale of surface activity in short-period binaries last from several up to a few hundreds of orbi ...
Accreting millisecond X-ray pulsars: a search for pulsed radio
... in its core at the end of its life. A typical neutron star has a mass between 1 M⊙ – 2.1 M⊙ , with a corresponding radius range of 8 – 15 km and then a resulting central density of 1014 −1015 g/cm3 (Lattimer & Prakash 2007). The combination of high mass and small size results in an extremely large g ...
... in its core at the end of its life. A typical neutron star has a mass between 1 M⊙ – 2.1 M⊙ , with a corresponding radius range of 8 – 15 km and then a resulting central density of 1014 −1015 g/cm3 (Lattimer & Prakash 2007). The combination of high mass and small size results in an extremely large g ...
Structure of the hot object in the symbiotic prototype Z And during its
... Cassegrain focus of the 1.82-m telescope at Mt. Ekar. Two very different exposures of 120 and 3 600 s were applied to obtain a well defined Hα profile and the underlying continuum. The RES orders were straightened through the software developed at the Astronomical Observatory of Capodimonte in Napol ...
... Cassegrain focus of the 1.82-m telescope at Mt. Ekar. Two very different exposures of 120 and 3 600 s were applied to obtain a well defined Hα profile and the underlying continuum. The RES orders were straightened through the software developed at the Astronomical Observatory of Capodimonte in Napol ...
Gamma-ray burst investigation via polarimetry and spectroscopy
... emission of electrons and protons: It is very probable that particles are accelerated to very high energies close to the emission site. This could either be in shock waves, where the Fermi mechanisms or other plasma instabilities act, or in magnetic reconnection sites. Therefore, it is likely that t ...
... emission of electrons and protons: It is very probable that particles are accelerated to very high energies close to the emission site. This could either be in shock waves, where the Fermi mechanisms or other plasma instabilities act, or in magnetic reconnection sites. Therefore, it is likely that t ...
Debris disks: seeing dust, thinking of planetesimals and planets
... Abstract Debris disks are optically thin, almost gas-free dusty disks observed around a significant fraction of main-sequence stars older than about 10 Myr. Since the circumstellar dust is short-lived, the very existence of these disks is considered as evidence that dust-producing planetesimals are ...
... Abstract Debris disks are optically thin, almost gas-free dusty disks observed around a significant fraction of main-sequence stars older than about 10 Myr. Since the circumstellar dust is short-lived, the very existence of these disks is considered as evidence that dust-producing planetesimals are ...
Digital Universe Guide - American Museum of Natural History
... 2. Unzip the downloaded file if your operating system does not unpack it automatically. (On Mac OS X, the file will appear as a mounted disk on your system.) 3. Optional: Move the resulting Digital Universe folder to any location in your file system. (The download is completely self-contained and do ...
... 2. Unzip the downloaded file if your operating system does not unpack it automatically. (On Mac OS X, the file will appear as a mounted disk on your system.) 3. Optional: Move the resulting Digital Universe folder to any location in your file system. (The download is completely self-contained and do ...
Stellar Populations of Dwarf Elliptical Galaxies: UBVRI Photometry
... giant elliptical galaxies in the Virgo Cluster. These observations confirm the marked difference in stellar population and stellar distribution between dwarf and giant elliptical galaxies and further substantiate the need for alternative evolutionary scenarios for the lowest mass cluster galaxies. W ...
... giant elliptical galaxies in the Virgo Cluster. These observations confirm the marked difference in stellar population and stellar distribution between dwarf and giant elliptical galaxies and further substantiate the need for alternative evolutionary scenarios for the lowest mass cluster galaxies. W ...
Radiative hydrodynamics simulations of red supergiant stars. III
... The top panel of Fig. 5 shows the temporal photocenter displacement over the ≈ 5 years of simulation, which is comparable to the total length of the Gaia mission. As seen in the Figure, for t < 22 yr, the random displacement is small and increases to a maximum value of 0.30 AU at t ∼ 23 yr. In relat ...
... The top panel of Fig. 5 shows the temporal photocenter displacement over the ≈ 5 years of simulation, which is comparable to the total length of the Gaia mission. As seen in the Figure, for t < 22 yr, the random displacement is small and increases to a maximum value of 0.30 AU at t ∼ 23 yr. In relat ...
A UNIQUE SOLUTION OF PLANET AND STAR PARAMETERS
... Follow-up mass determination by radial velocity measurements is needed for planet transit candidates because late M dwarfs (M 80 MJ), brown dwarfs (13 MJ < M < 80 MJ), and gas giant planets (M 13 MJ) are all of similar sizes. This is due to a coincidental balance between Coulomb forces (which ca ...
... Follow-up mass determination by radial velocity measurements is needed for planet transit candidates because late M dwarfs (M 80 MJ), brown dwarfs (13 MJ < M < 80 MJ), and gas giant planets (M 13 MJ) are all of similar sizes. This is due to a coincidental balance between Coulomb forces (which ca ...
On the importance of using appropriate spectral models to derive .
... proposed, based on combination of stellar population synthesis and photoionization codes (e.g., Charlot & Longhetti 2001; Groves et al. 2008). Pacifici et al. (2012) provide the sophisticated modelling framework required to interpret multi-wavelength photometric and spectroscopic galaxy observations ...
... proposed, based on combination of stellar population synthesis and photoionization codes (e.g., Charlot & Longhetti 2001; Groves et al. 2008). Pacifici et al. (2012) provide the sophisticated modelling framework required to interpret multi-wavelength photometric and spectroscopic galaxy observations ...
the article as PDF - Project VS
... solid line represents the theoretical LITE variation caused by a 3rd body and the O-C residuals obtained after the subtraction of LITE (lower part). For details, please refer to (Zasche, Liakos et al., 2009) ...
... solid line represents the theoretical LITE variation caused by a 3rd body and the O-C residuals obtained after the subtraction of LITE (lower part). For details, please refer to (Zasche, Liakos et al., 2009) ...
planetary construction zones in occultation: discovery of an
... for additional minima at different orbital phases when one of the stars is hidden behind them.” In this paper we present the discovery of a solar mass pre-main sequence non-accreting star exhibiting a long, unusual eclipse similar to those seen in EE Cep and ǫ Aurigae. The mass of the star and lack ...
... for additional minima at different orbital phases when one of the stars is hidden behind them.” In this paper we present the discovery of a solar mass pre-main sequence non-accreting star exhibiting a long, unusual eclipse similar to those seen in EE Cep and ǫ Aurigae. The mass of the star and lack ...
Dark matter scaling relations and the assembly epoch of Coma early
... Axisymmetric, orbit-based dynamical models are used to derive dark matter scaling relations for Coma early-type galaxies. From faint to bright galaxies halo core-radii and asymptotic circular velocities increase. Compared to spirals of the same brightness, the majority of Coma early-types – those wi ...
... Axisymmetric, orbit-based dynamical models are used to derive dark matter scaling relations for Coma early-type galaxies. From faint to bright galaxies halo core-radii and asymptotic circular velocities increase. Compared to spirals of the same brightness, the majority of Coma early-types – those wi ...
Swift and NuSTAR observations of XTE J1859+083
... The common way to create a NS is when a high mass star ends its life in a Type-II supernova witch a progenitor mass of at least 8 M (Smartt, 2009). Once a gas cloud collapses under gravitational force and forms a ball of hot plasma, fusing hydrogen to helium in its core, a star is born. The evoluti ...
... The common way to create a NS is when a high mass star ends its life in a Type-II supernova witch a progenitor mass of at least 8 M (Smartt, 2009). Once a gas cloud collapses under gravitational force and forms a ball of hot plasma, fusing hydrogen to helium in its core, a star is born. The evoluti ...
Here - NASA/IPAC Extragalactic Database
... H ii regions are ionized clouds of gas associated with zones of recent star formation. They are powered by one, a few, or a cluster of massive stars (depending on the resolution at which one is working). The effective temperatures T? of the ionizing stars lie in the range 35 000 – 50 000 K. The nebu ...
... H ii regions are ionized clouds of gas associated with zones of recent star formation. They are powered by one, a few, or a cluster of massive stars (depending on the resolution at which one is working). The effective temperatures T? of the ionizing stars lie in the range 35 000 – 50 000 K. The nebu ...
Summary of dynamics of the regular heptagon: N =7
... D’s region spans 3 forward edges since it is step -3. This span is maximal for N = 7 so D has the largest possible measure. The development of S[1] and S[2] are similar, but complicated by the congestion of the ‘inner star’ region. In all cases the shear is the same, so the centers of these regions ...
... D’s region spans 3 forward edges since it is step -3. This span is maximal for N = 7 so D has the largest possible measure. The development of S[1] and S[2] are similar, but complicated by the congestion of the ‘inner star’ region. In all cases the shear is the same, so the centers of these regions ...
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.