5 Report of the Panel on Stars and Stellar Evolution
... How Do Rotation and Magnetic Fields Affect Stars? There’s an old chestnut about a dozing theorist at the weekly colloquium who opens his eyes at the end of every talk and rouses himself to ask, to great approbation for his subliminal understanding, “Yes, all very interesting, but what about rotatio ...
... How Do Rotation and Magnetic Fields Affect Stars? There’s an old chestnut about a dozing theorist at the weekly colloquium who opens his eyes at the end of every talk and rouses himself to ask, to great approbation for his subliminal understanding, “Yes, all very interesting, but what about rotatio ...
MEarth
... much more frequently. At 0.074 AU from the M5, a planet would transit once every 14.5 days, compared to 1 year for the Earth-Sun system. This is critical for detectability, as dramatically less observational time is required to achieve a transit detection. 3. The small radii of M dwarfs lead to much ...
... much more frequently. At 0.074 AU from the M5, a planet would transit once every 14.5 days, compared to 1 year for the Earth-Sun system. This is critical for detectability, as dramatically less observational time is required to achieve a transit detection. 3. The small radii of M dwarfs lead to much ...
Super-Eddington outburst in a binary system: V4641 Sgr Mikhail Revnivtsev, Marat Gilfanov
... • We argue that V4641 Sgr in Sep. 1999 demonstrated an episode of super-Eddington accretion • During this episode a powerful expended evelope was formed • When the accretion rate decreased the envelope vanished • X-ray observations support this picture: we have detected the change in the X-ray absor ...
... • We argue that V4641 Sgr in Sep. 1999 demonstrated an episode of super-Eddington accretion • During this episode a powerful expended evelope was formed • When the accretion rate decreased the envelope vanished • X-ray observations support this picture: we have detected the change in the X-ray absor ...
It is now recognized that the vast majority of ellipticals are of
... • The dust lanes seen in E galaxies imply that the absorbing material is distributed in rings or disks. Dust lanes may be aligned with either the major or minor axes, or they may be warped. • E galaxies contain modest amounts of cool and warm gas, although not as much as is found in S galaxies. A fe ...
... • The dust lanes seen in E galaxies imply that the absorbing material is distributed in rings or disks. Dust lanes may be aligned with either the major or minor axes, or they may be warped. • E galaxies contain modest amounts of cool and warm gas, although not as much as is found in S galaxies. A fe ...
PPT presentation
... Monk et al. (1988) analysed 3.9m AAT spectra of 21 SMC and 50 LMC PNe. They found that the PN and HII region abundances of oxygen and neon agreed within the same galaxy but that the PN nitrogen was enhanced by 0.9 dex in the SMC and LMC. Interpreted as due to CN cycle processing of almost all of th ...
... Monk et al. (1988) analysed 3.9m AAT spectra of 21 SMC and 50 LMC PNe. They found that the PN and HII region abundances of oxygen and neon agreed within the same galaxy but that the PN nitrogen was enhanced by 0.9 dex in the SMC and LMC. Interpreted as due to CN cycle processing of almost all of th ...
Masses of Dwarf Satellites of the Milky Way
... Q, for 526 subhaloes in the main halo of the Aq-A-1 simulation. haloes considered contain between 20 000 and nearly ∼10 million . The lines in different colours show averages in logarithmic mass each of the three profiles. ...
... Q, for 526 subhaloes in the main halo of the Aq-A-1 simulation. haloes considered contain between 20 000 and nearly ∼10 million . The lines in different colours show averages in logarithmic mass each of the three profiles. ...
The Evolution of Molecular Clouds
... The above calculations may not, however, be very relevant to real molecular clouds, most of which are far from spherical and are rotating only rather slowly (Goodman et al. 1993). The probably more realistic case of the collapse of an elongated cylindrical cloud has been studied numerically by Basti ...
... The above calculations may not, however, be very relevant to real molecular clouds, most of which are far from spherical and are rotating only rather slowly (Goodman et al. 1993). The probably more realistic case of the collapse of an elongated cylindrical cloud has been studied numerically by Basti ...
Document
... Color-Magnitude sequence: zero-point, slope and scatter passive evolution of stellar populations formed at z>2-3. Slope is primarily driven by mass-metallicity relation. Morphologically (HST)-selected Es and S0s (Bower et al. 1992, Aragon-Salamanca et al. 1993, Rakos et al. 1995, Stanford et al. 199 ...
... Color-Magnitude sequence: zero-point, slope and scatter passive evolution of stellar populations formed at z>2-3. Slope is primarily driven by mass-metallicity relation. Morphologically (HST)-selected Es and S0s (Bower et al. 1992, Aragon-Salamanca et al. 1993, Rakos et al. 1995, Stanford et al. 199 ...
Emergency Land Navigation
... Earth’s interior is a natural magnet, thus we can use the compass to determine our Magnetic North and South. After which, we can deduce the geographic North and South with some basic calculations, from the information taken from maps and charts. Just like a map with grid coordinates, we have conveni ...
... Earth’s interior is a natural magnet, thus we can use the compass to determine our Magnetic North and South. After which, we can deduce the geographic North and South with some basic calculations, from the information taken from maps and charts. Just like a map with grid coordinates, we have conveni ...
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 ...
Rocky planetesimals as the origin of metals in DZ stars
... where hydrogen is detected or inferred (Dufour et al. 2007) versus height above the Galactic mid-plane and tangential speed. No obvious pattern is seen, although there may be a higher density of DZA stars near the Galactic disc and perhaps also towards more modest speeds, but the former may be an ob ...
... where hydrogen is detected or inferred (Dufour et al. 2007) versus height above the Galactic mid-plane and tangential speed. No obvious pattern is seen, although there may be a higher density of DZA stars near the Galactic disc and perhaps also towards more modest speeds, but the former may be an ob ...
Mn, Cu, and Zn abundances in barium stars and their correlations
... intermediate mass AGB stars, and the weak component of the s-process, thought to be sited at He-burning cores of M ≥ 10 M stars (see Raiteri et al. 1993; Matteucci et al. 1993; Mishenina et al. 2002, and references therein). Even though their positions in the periodic table are contiguous, their be ...
... intermediate mass AGB stars, and the weak component of the s-process, thought to be sited at He-burning cores of M ≥ 10 M stars (see Raiteri et al. 1993; Matteucci et al. 1993; Mishenina et al. 2002, and references therein). Even though their positions in the periodic table are contiguous, their be ...
UK Exoplanet community meeting 2017
... stars and in developing solutions to enable the detection and characterisation of superEarths and Earths. The aim of this session is to bring the community together to share both published and unpublished information, to dispel some common misconceptions and myths in the field and to initiate/streng ...
... stars and in developing solutions to enable the detection and characterisation of superEarths and Earths. The aim of this session is to bring the community together to share both published and unpublished information, to dispel some common misconceptions and myths in the field and to initiate/streng ...
THE N/O RATIO IN EARLY B-TYPE MAIN SEQUENCE STARS AS
... This paper is based on previous studies of MS B-stars which were published between 2000 and 2008 by Lyubimkov, et al. [8-12]. High resolution spectra for more than 100 MS B-stars were obtained [8] at two observatories, the Crimean Astrophysical Observatory and the MacDonald Observatory of the Unive ...
... This paper is based on previous studies of MS B-stars which were published between 2000 and 2008 by Lyubimkov, et al. [8-12]. High resolution spectra for more than 100 MS B-stars were obtained [8] at two observatories, the Crimean Astrophysical Observatory and the MacDonald Observatory of the Unive ...
Lokal fulltext - Chalmers Publication Library
... only in the spectral energy distribution (SED) they could not infer any shape. The excess is beyond 12 µm and peaks close to 60 µm. They interpreted this as emission from solid particles at 85 AU from the star, distributed in either a shell or a ring (see Figure 1.1). Since such excess first was obs ...
... only in the spectral energy distribution (SED) they could not infer any shape. The excess is beyond 12 µm and peaks close to 60 µm. They interpreted this as emission from solid particles at 85 AU from the star, distributed in either a shell or a ring (see Figure 1.1). Since such excess first was obs ...
ABSTRACT Exoplanet Habitability and an Analysis of Gliese 436 b
... presence in DNA and proteins.11 Remember that without the presence of water though, these building blocks will not lead to the development of life. Along with water and these building blocks, UV radiation and greenhouse gases must be considered. If too much radiation reaches the exoplanet’s surface, ...
... presence in DNA and proteins.11 Remember that without the presence of water though, these building blocks will not lead to the development of life. Along with water and these building blocks, UV radiation and greenhouse gases must be considered. If too much radiation reaches the exoplanet’s surface, ...
Multiplicity in Early Stellar Evolution
... While powerful theoretical tools now exist, along with widespread access to large computational clusters, the huge volume of parameter space that needs to be explored has to date prevented a comprehensive theoretical picture from emerging. Nevertheless, it is clear that in spite of the various magne ...
... While powerful theoretical tools now exist, along with widespread access to large computational clusters, the huge volume of parameter space that needs to be explored has to date prevented a comprehensive theoretical picture from emerging. Nevertheless, it is clear that in spite of the various magne ...
on the pms star hbc 498 and its associated nebulous stars1
... HBC 495 and DL Ori/G2 have Li Iλ6708 Å strong in absorption (see Fig. 2 and Table 3), with equivalent widths stronger than the richest Li I stars with similar spectral types in the Pleiades cluster (i.e., “Li I rich stars”). The Li I line is apparently present in the spectrum of HBC 496, but the sp ...
... HBC 495 and DL Ori/G2 have Li Iλ6708 Å strong in absorption (see Fig. 2 and Table 3), with equivalent widths stronger than the richest Li I stars with similar spectral types in the Pleiades cluster (i.e., “Li I rich stars”). The Li I line is apparently present in the spectrum of HBC 496, but the sp ...
The white dwarf population within 40 pc of the Sun
... (black dots) and the corresponding selection criteria (red dashed lines) are displayed. As can be seen, the overall effect of this selection criterion is that the selected sample is, on average, redder than the population from which it is drawn, independent of the adopted age of the disk. Additionall ...
... (black dots) and the corresponding selection criteria (red dashed lines) are displayed. As can be seen, the overall effect of this selection criterion is that the selected sample is, on average, redder than the population from which it is drawn, independent of the adopted age of the disk. Additionall ...
Unraveling the Helix Nebula: Its Structure and Knots
... use the coordinate based system introduced in OB1997, thus avoiding the confusion of a discovery-time based system. We give figures labeling features at decreasing surface brightness and increasing size in Figure 3, Figure 6, and Figure 17. We describe the new high resolution HST and broader field ...
... use the coordinate based system introduced in OB1997, thus avoiding the confusion of a discovery-time based system. We give figures labeling features at decreasing surface brightness and increasing size in Figure 3, Figure 6, and Figure 17. We describe the new high resolution HST and broader field ...
Lyra
Lyra (/ˈlaɪərə/; Latin for lyre, from Greek λύρα) is a small constellation. It is one of 48 listed by the 2nd century astronomer Ptolemy, and is one of the 88 constellations recognized by the International Astronomical Union. Lyra was often represented on star maps as a vulture or an eagle carrying a lyre, and hence sometimes referred to as Aquila Cadens or Vultur Cadens. Beginning at the north, Lyra is bordered by Draco, Hercules, Vulpecula, and Cygnus. Lyra is visible from the northern hemisphere from spring through autumn, and nearly overhead, in temperate latitudes, during the summer months. From the southern hemisphere, it is visible low in the northern sky during the winter months.The lucida or brightest star—and one of the brightest stars in the sky—is the white main sequence star Vega, a corner of the Summer Triangle. Beta Lyrae is the prototype of a class of stars known as Beta Lyrae variables, binary stars so close to each other that they become egg-shaped and material flows from one to the other. Epsilon Lyrae, known informally as the Double Double, is a complex multiple star system. Lyra also hosts the Ring Nebula, the second-discovered and best-known planetary nebula.