WR25 Carina Nebula
... GSE-X points towards the sun. GSE-X-GSE-Y plane is the plane of the ecliptic. GSE-Z is towards the north pole. Red indicates higher values. ...
... GSE-X points towards the sun. GSE-X-GSE-Y plane is the plane of the ecliptic. GSE-Z is towards the north pole. Red indicates higher values. ...
Astronomy Astrophysics First detection of the field star overdensity in the Perseus... &
... the two sets of physical parameters. This cleanest sample contains 8328 stars and is named CS-MB or CS-EC depending on whether their physical parameters were computed using the MB or EC method (see Fig. 1). This sample contains stars with more accurate SPP data, but has fewer statistics owing to the ...
... the two sets of physical parameters. This cleanest sample contains 8328 stars and is named CS-MB or CS-EC depending on whether their physical parameters were computed using the MB or EC method (see Fig. 1). This sample contains stars with more accurate SPP data, but has fewer statistics owing to the ...
Tycho Brahe
... producing a family of his own. • According to one account, Otto and Beate promised Jörgen their first son, but changed their minds. • Jörgen kidnapped Tycho after 1 year, while Beate was pregnant with their second. ...
... producing a family of his own. • According to one account, Otto and Beate promised Jörgen their first son, but changed their minds. • Jörgen kidnapped Tycho after 1 year, while Beate was pregnant with their second. ...
Hot subdwarf stars-galactic orbits and distribution perpendicular to
... epoch position, we are not able to calculate proper motion errors. An indication of the proper motion uncertainty may be the uncertainty of the zero point shift, representing a lower limit to our errors. In Table 2, δ(µα cosδ) and δ(µδ ) designate the mean uncertainty of the zero point shift represe ...
... epoch position, we are not able to calculate proper motion errors. An indication of the proper motion uncertainty may be the uncertainty of the zero point shift, representing a lower limit to our errors. In Table 2, δ(µα cosδ) and δ(µδ ) designate the mean uncertainty of the zero point shift represe ...
Nucleosynthesis and Chemical Evolution of Oxygen
... of one stage serve as the fuel for the next. This sequence of burning stages progresses until either electron degeneracy replaces thermal pressure to support the star or the star burns the nuclei all the way to iron from which no more nuclear energy can be extracted by fusion The first nuclear fuel ...
... of one stage serve as the fuel for the next. This sequence of burning stages progresses until either electron degeneracy replaces thermal pressure to support the star or the star burns the nuclei all the way to iron from which no more nuclear energy can be extracted by fusion The first nuclear fuel ...
On the interpretation of stellar disc observations in terms of diameters
... factor when cos u gets very close to zero. The (essentially coinciding) positions of these inflection points of monochromatic intensity CLVs define a unique intensity radius (Baschek et al. 1991) of a very-compact-atmosphere star and are conventionally used for determining the photospheric radius of ...
... factor when cos u gets very close to zero. The (essentially coinciding) positions of these inflection points of monochromatic intensity CLVs define a unique intensity radius (Baschek et al. 1991) of a very-compact-atmosphere star and are conventionally used for determining the photospheric radius of ...
Chemical analysis of 24 dusty (pre-) main
... as a class in 1960 by Herbig, based on three observational criteria: the stars have spectral type A or earlier, display emission lines, and illuminate a bright reflection nebula in their immediate vicinity. Later on other observational criteria were proposed. Finkenzeller & Mundt (1984) mentioned th ...
... as a class in 1960 by Herbig, based on three observational criteria: the stars have spectral type A or earlier, display emission lines, and illuminate a bright reflection nebula in their immediate vicinity. Later on other observational criteria were proposed. Finkenzeller & Mundt (1984) mentioned th ...
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 Extragalactic Group of MPE and USM
... of Massive Galaxies in the FORS Deep and GOODS South fields • Study evolution of galaxies with broadband deep U to K surveys. • LFs, Mass Functions, SFRs do not require spectroscopy but can be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter lumin ...
... of Massive Galaxies in the FORS Deep and GOODS South fields • Study evolution of galaxies with broadband deep U to K surveys. • LFs, Mass Functions, SFRs do not require spectroscopy but can be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter lumin ...
21 -26 August University of Exeter
... Investigating the dynamics of the interstellar medium (ISM) is key to gaining insight into the formation of starforming filaments in molecular clouds (MCs). A plethora of numerical and analytical models associate the origin of this filamentary structure to the interplay between self-gravity and magn ...
... Investigating the dynamics of the interstellar medium (ISM) is key to gaining insight into the formation of starforming filaments in molecular clouds (MCs). A plethora of numerical and analytical models associate the origin of this filamentary structure to the interplay between self-gravity and magn ...
What Are the Faint X-ray Transients Near the Galactic Center?
... • The long, slow transient to the left has a soft spectrum reminiscent of transient magnetars. ...
... • The long, slow transient to the left has a soft spectrum reminiscent of transient magnetars. ...
Review: How does a star`s mass determine its life story?
... Roche lobes: over/under surface where the gravity of two stars balance. © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley ...
... Roche lobes: over/under surface where the gravity of two stars balance. © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley ...
PP Chapter 28 Text
... F = G(m1 m2)/d2. Letting this equation guide our thinking, we see that none of its terms differ. Although the density of the black hole has greatly increased, its mass is the same before and after collapse. Because the mass of Earth and the solar black hole are the same, and distance between cente ...
... F = G(m1 m2)/d2. Letting this equation guide our thinking, we see that none of its terms differ. Although the density of the black hole has greatly increased, its mass is the same before and after collapse. Because the mass of Earth and the solar black hole are the same, and distance between cente ...
The white dwarf population within 40 pc of the Sun
... (black lines) compared to the observed luminosity function (red line). The solid line shows the luminosity function of the simulated white dwarf population when all the selection criteria have been considered, while the dashed line displays the luminosity function of the entire sample. Bottom panel: ...
... (black lines) compared to the observed luminosity function (red line). The solid line shows the luminosity function of the simulated white dwarf population when all the selection criteria have been considered, while the dashed line displays the luminosity function of the entire sample. Bottom panel: ...
Document
... break technique in combination with the new generation of 8- to 10-m telescopes made it possible to identify significant samples of high-redshift objects. Lyman Break Galaxies (LBGs) are color-selected, luminous, star forming galaxies that emitted their light more than 10 billion years ago, e.g., at ...
... break technique in combination with the new generation of 8- to 10-m telescopes made it possible to identify significant samples of high-redshift objects. Lyman Break Galaxies (LBGs) are color-selected, luminous, star forming galaxies that emitted their light more than 10 billion years ago, e.g., at ...
A physical interpretation of the `red Sirius` anomaly
... other historical evidence for a red Sirius seems both reliable and unambiguous [see Ceragioli (1995) for a critical, in-depth review]. Babylonian cuneiform texts, and the writings of classical GrecoRoman authors, including Cicero, Horace, Seneca and Ptolemy, refer consistently to Sirius as a red or ...
... other historical evidence for a red Sirius seems both reliable and unambiguous [see Ceragioli (1995) for a critical, in-depth review]. Babylonian cuneiform texts, and the writings of classical GrecoRoman authors, including Cicero, Horace, Seneca and Ptolemy, refer consistently to Sirius as a red or ...
Mass loss of massive stars near the Eddington luminosity by core
... shows tdyn (10 R ) for given R and ΔM, and the righthand panel shows tdyn (100 R ). We can see that material ejected from a star with R ∼ R , which is a typical radius of WR stars, can easily reach above 10 R within several days and above 100 R in ∼10 days. Material ejected from larger stars ...
... shows tdyn (10 R ) for given R and ΔM, and the righthand panel shows tdyn (100 R ). We can see that material ejected from a star with R ∼ R , which is a typical radius of WR stars, can easily reach above 10 R within several days and above 100 R in ∼10 days. Material ejected from larger stars ...
The cosmological significance of high
... could be as large as 6.5 kpc. Blitz et al. (1999) additionally pointed out that the velocity of Complex H is too large for it to be in circular rotation around the Galaxy at any distance. They further argued that the lack of any observational evidence for an interaction between Complex H and the int ...
... could be as large as 6.5 kpc. Blitz et al. (1999) additionally pointed out that the velocity of Complex H is too large for it to be in circular rotation around the Galaxy at any distance. They further argued that the lack of any observational evidence for an interaction between Complex H and the int ...
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.