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IAC_L5_bulge_GALAH
... buckling into the peanut structure, so the components A-E are trapped relics of the Galactic disk and halo from that time. The instability process generated a mapping of the stars of the early disk into the boxy/peanut structure. In this way, the bulge preserves a dynamical imprint of the chemical d ...
... buckling into the peanut structure, so the components A-E are trapped relics of the Galactic disk and halo from that time. The instability process generated a mapping of the stars of the early disk into the boxy/peanut structure. In this way, the bulge preserves a dynamical imprint of the chemical d ...
FIRST DETECTION OF KRYPTON AND XENON IN A WHITE DWARF
... level energies from Biémont et al. (2005). f values were mainly taken from that source, too, and from Reyna Almandos et al. (2001). In total, f values are unknown for 389 of the 887 included line transitions. NIST lists 16 lines in the FUSE range. For the line fit, we omit three weak ones that are ...
... level energies from Biémont et al. (2005). f values were mainly taken from that source, too, and from Reyna Almandos et al. (2001). In total, f values are unknown for 389 of the 887 included line transitions. NIST lists 16 lines in the FUSE range. For the line fit, we omit three weak ones that are ...
gravitational collapse to black holes
... If the central pressure inside the star is high enough (due to higher mass), the star will start burning helium at its core. If that fuel is exhausted, it will continue with carbon and so on ...
... If the central pressure inside the star is high enough (due to higher mass), the star will start burning helium at its core. If that fuel is exhausted, it will continue with carbon and so on ...
Asymptotic Giant Branch stars viewed up-close and far-off
... Stars form in dense molecular cores inside interstellar clouds of gas and dust. At some point the dense cores are overcome by their own gravity and start to collapse. As more material collapses onto the central region, the pressure and temperature in the core increase, eventually halting the collaps ...
... Stars form in dense molecular cores inside interstellar clouds of gas and dust. At some point the dense cores are overcome by their own gravity and start to collapse. As more material collapses onto the central region, the pressure and temperature in the core increase, eventually halting the collaps ...
Kepler-21b: A Rocky Planet Around a V= 8.25 Magnitude Star
... sculpted by photo-evaporation (e. g. Lopez et al. 2012; Lopez & Fortney 2013; Owen & Wu 2013), or else by some other comparable process like atmospheric erosion by impacts (e. g. Inamdar & Schlichting 2015; Schlichting et al. 2015). Thus, while it is possible that the short-period rocky planets simp ...
... sculpted by photo-evaporation (e. g. Lopez et al. 2012; Lopez & Fortney 2013; Owen & Wu 2013), or else by some other comparable process like atmospheric erosion by impacts (e. g. Inamdar & Schlichting 2015; Schlichting et al. 2015). Thus, while it is possible that the short-period rocky planets simp ...
PLANETS AND INFRARED EXCESSES: PRELIMINARY RESULTS
... ring was chosen. Because the accuracy of the 70 m data is limited by background noise, rather than instrumental effects, such a large aperture contains an undesirable amount of sky fluctuations. In order to maximize S/ N, a smaller aperture is more appropriate at 70 m—just 1.5 pixels in radius. Wi ...
... ring was chosen. Because the accuracy of the 70 m data is limited by background noise, rather than instrumental effects, such a large aperture contains an undesirable amount of sky fluctuations. In order to maximize S/ N, a smaller aperture is more appropriate at 70 m—just 1.5 pixels in radius. Wi ...
PDF only - at www.arxiv.org.
... 2008; Garcia Muñoz, 2007; Penz et al., 2008; Guo 2011, 2013; Murray-Clay et al., 2009; Koskinen et al., 2013a, 2013b). Garcia-Muñoz (2007) modelled the physical and chemical aeronomy of HD 209458b, and concluded that beyond a few planetary radii all elements are strongly ionized, assuming that the e ...
... 2008; Garcia Muñoz, 2007; Penz et al., 2008; Guo 2011, 2013; Murray-Clay et al., 2009; Koskinen et al., 2013a, 2013b). Garcia-Muñoz (2007) modelled the physical and chemical aeronomy of HD 209458b, and concluded that beyond a few planetary radii all elements are strongly ionized, assuming that the e ...
On the evolution and fate of supermassive stars
... Context. We study the evolution and fate of solar composition super-massive stars in the mass range 60 — 1000 M⊙ . Our study is relevant for very massive objects observed in young stellar complexes as well as for super-massive stars that could potentially form through runaway stellar collisions. Aim ...
... Context. We study the evolution and fate of solar composition super-massive stars in the mass range 60 — 1000 M⊙ . Our study is relevant for very massive objects observed in young stellar complexes as well as for super-massive stars that could potentially form through runaway stellar collisions. Aim ...
IDENTIFICATION OF MAIN-SEQUENCE STARS WITH MID
... most found using high-resolution stellar spectroscopy capable of detecting Doppler shifts in the parent star. However, the process or processes by which these planets form is still unknown. Planetesimals may originate in circumstellar disks, formed as a by-product of star formation. The evolutionary ...
... most found using high-resolution stellar spectroscopy capable of detecting Doppler shifts in the parent star. However, the process or processes by which these planets form is still unknown. Planetesimals may originate in circumstellar disks, formed as a by-product of star formation. The evolutionary ...
Properties of Galactic B supergiants
... (Crowther & Dessart 1998). HD 97950 closely resembles R136 in the LMC (Walborn 1973; Moffat 1983), yet unlike R136, it does not possess an extensive halo of earlier phases of massive star formation. Perhaps Sher 25 is a foreground object, which may plausibly be inferred from the presence of other st ...
... (Crowther & Dessart 1998). HD 97950 closely resembles R136 in the LMC (Walborn 1973; Moffat 1983), yet unlike R136, it does not possess an extensive halo of earlier phases of massive star formation. Perhaps Sher 25 is a foreground object, which may plausibly be inferred from the presence of other st ...
Cosmology
... • Can we see galaxies receding faster than light ? • Why is there a cosmic redshift ? • How large is the observable universe ? • Do objects inside the universe expand, too ? ...
... • Can we see galaxies receding faster than light ? • Why is there a cosmic redshift ? • How large is the observable universe ? • Do objects inside the universe expand, too ? ...
Dynamics of Stars and Black Holes in Dense Stellar Systems:
... Or, to say it in a different way (more physical?) ⇒ POTENTIAL WELL BECOMES PERMANENTLY SHALLOWER ⇒ AND SYSTEM EXPANDS (*) (*) IF the system expands, it becomes LESS DENSE ⇒ lower density implies LESS two-body encounters ⇒ stars exchange less energy and become dynamically cooler ⇒ gravothermal CATAST ...
... Or, to say it in a different way (more physical?) ⇒ POTENTIAL WELL BECOMES PERMANENTLY SHALLOWER ⇒ AND SYSTEM EXPANDS (*) (*) IF the system expands, it becomes LESS DENSE ⇒ lower density implies LESS two-body encounters ⇒ stars exchange less energy and become dynamically cooler ⇒ gravothermal CATAST ...
A hypervelocity star from the Large Magellanic Cloud
... initial velocity between the binary and the single star as the total energy of the system is dominated by the binding energy of the binary rather than by the kinetic energy of the incoming star. Additional experiments performed with initial velocities of 5 and 10 km s−1 showed no appreciable differe ...
... initial velocity between the binary and the single star as the total energy of the system is dominated by the binding energy of the binary rather than by the kinetic energy of the incoming star. Additional experiments performed with initial velocities of 5 and 10 km s−1 showed no appreciable differe ...
Final Paper Template for the 5th Southeast Asian Forum
... tidal field, leave behind only few members and known as Open Cluster Remnants (OCR). They have very low surface density but high binary fraction. One of well-studied OCRs is NGC 1901 (α = 5h18m15s and δ = −68°26’12”; l = 279.022° and b = −33.603°). This middle aged (approximately 400 to 850 Myr) clu ...
... tidal field, leave behind only few members and known as Open Cluster Remnants (OCR). They have very low surface density but high binary fraction. One of well-studied OCRs is NGC 1901 (α = 5h18m15s and δ = −68°26’12”; l = 279.022° and b = −33.603°). This middle aged (approximately 400 to 850 Myr) clu ...
the challenge of wide-field transit surveys: the case of
... moon. Nevertheless, the photometry is good enough to ascertain that the depth of the transit-like events is equal within the observational errors in all three filters. A statistically significant difference in the transit depths (after accounting for limb darkening) would have rejected this object a ...
... moon. Nevertheless, the photometry is good enough to ascertain that the depth of the transit-like events is equal within the observational errors in all three filters. A statistically significant difference in the transit depths (after accounting for limb darkening) would have rejected this object a ...
Planetary System Disruption by Galactic
... approximate age of our galaxy’s thin disk). Even though binaries with smaller semimajor axes are less affected by galactic perturbations, Figure 2a shows the influence of binary semimajor axis on planetary instability rates is weak. This is because tighter binaries make pericenter passages at a high ...
... approximate age of our galaxy’s thin disk). Even though binaries with smaller semimajor axes are less affected by galactic perturbations, Figure 2a shows the influence of binary semimajor axis on planetary instability rates is weak. This is because tighter binaries make pericenter passages at a high ...
Galaxies
... spectrum of the star, they found something completely unexpected: the spectrum was flat with several unexpected, and totally unexplainable, emission lines. The object remained a mystery until similar but brighter object, 3C 273, was discovered in 1963. Astronomers noticed that 3C 273 had a normal sp ...
... spectrum of the star, they found something completely unexpected: the spectrum was flat with several unexpected, and totally unexplainable, emission lines. The object remained a mystery until similar but brighter object, 3C 273, was discovered in 1963. Astronomers noticed that 3C 273 had a normal sp ...
Stars and Galaxies
... close to one another. You can see that some of the stars are brighter than others, but you can’t see how far they are from you or from each other. Usually, they lie at greatly different distances and just happen to line up and form a pattern. In Figure 1, three constellations are shown with some of ...
... close to one another. You can see that some of the stars are brighter than others, but you can’t see how far they are from you or from each other. Usually, they lie at greatly different distances and just happen to line up and form a pattern. In Figure 1, three constellations are shown with some of ...
On the onset of runaway stellar collisions in dense star clusters I
... studying young star clusters such as R136, MGG11 and Arches (Massey & Hunter 1998; Figer et al. 2002; McCrady et al. 2005), and young star clusters are thought to be born with high concentration (Merritt et al. 2004). In addition, high concentration is a necessary condition for clusters which can ex ...
... studying young star clusters such as R136, MGG11 and Arches (Massey & Hunter 1998; Figer et al. 2002; McCrady et al. 2005), and young star clusters are thought to be born with high concentration (Merritt et al. 2004). In addition, high concentration is a necessary condition for clusters which can ex ...
TRIFFID photometry of globular cluster cores – I. Photometric
... Cepheid of the W Vir type located some 13 arcsec from the centre, was detected only because it is brighter in the standard blue photographic passbands than any other star within 20 arcsec of the centre (see Fusi Pecci et al. 1980 and references therein). Furthermore, the formation of close binaries ...
... Cepheid of the W Vir type located some 13 arcsec from the centre, was detected only because it is brighter in the standard blue photographic passbands than any other star within 20 arcsec of the centre (see Fusi Pecci et al. 1980 and references therein). Furthermore, the formation of close binaries ...
Chapter 9 Red Giant Evolution
... can no longer support itself, or the layers above, against gravity. • It begins to collapse on a Kelvin–Helmholtz timescale, which is – slow compared to the dynamical timescale but – rapid compared to the nuclear burning timescale that has governed the time spent on the main sequence. • The collapse ...
... can no longer support itself, or the layers above, against gravity. • It begins to collapse on a Kelvin–Helmholtz timescale, which is – slow compared to the dynamical timescale but – rapid compared to the nuclear burning timescale that has governed the time spent on the main sequence. • The collapse ...
fundamental properties of kepler planet- candidate
... published in separate studies). For 69 host stars short-cadence data were used, while 8 of them showed oscillations with νmax values low enough to allow a detection using long-cadence data. The final values for Δν and νmax are listed in Table 1 and were adopted from the method of Huber et al. (2009) ...
... published in separate studies). For 69 host stars short-cadence data were used, while 8 of them showed oscillations with νmax values low enough to allow a detection using long-cadence data. The final values for Δν and νmax are listed in Table 1 and were adopted from the method of Huber et al. (2009) ...
L133 VERY LARGE TELESCOPE SPECTRA OF CARBON STARS
... In general, stars are oxygen-rich when they enter the AGB phase. Third dredge-up leads to 12C enrichment in the atmospheres of AGB stars. If the C/O ratio exceeds unity after the third dredge-up, the star is classified as a carbon star. Theoretical models have predicted that the amount of 12C enrich ...
... In general, stars are oxygen-rich when they enter the AGB phase. Third dredge-up leads to 12C enrichment in the atmospheres of AGB stars. If the C/O ratio exceeds unity after the third dredge-up, the star is classified as a carbon star. Theoretical models have predicted that the amount of 12C enrich ...
Population synthesis of Be/white dwarf binaries in the Galaxy
... The calculations have been made using the Scenario Machine. The program Scenario Machine was described for the first time in a paper by Kornilov & Lipunov (1983). Recently a very detailed description of this program was given in a review by Lipunov et al. (1996). Here we will only describe some gene ...
... The calculations have been made using the Scenario Machine. The program Scenario Machine was described for the first time in a paper by Kornilov & Lipunov (1983). Recently a very detailed description of this program was given in a review by Lipunov et al. (1996). Here we will only describe some gene ...
Planetary nebula
![](https://commons.wikimedia.org/wiki/Special:FilePath/NGC6543.jpg?width=300)
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.