Chemical composition of halo and disk stars with
... were included, this gives a higher accuracy than area integration, which is more affected by blends in the outer parts of the lines. Altogether 13 halo stars and 16 disk stars were observed. Most of them have magnitudes between mV = 9 and 11. The S/N of the spectra ranges from about 180 in the centr ...
... were included, this gives a higher accuracy than area integration, which is more affected by blends in the outer parts of the lines. Altogether 13 halo stars and 16 disk stars were observed. Most of them have magnitudes between mV = 9 and 11. The S/N of the spectra ranges from about 180 in the centr ...
Was a cloud-cloud collision the trigger of the recent star formation in
... state. Again, we are only interested in the evolution of the clouds up to the point where star formation takes place. This renders a reasonable simplification given that we consider the structure of the gas prior to stellar feedback. 3.2. Initial conditions ...
... state. Again, we are only interested in the evolution of the clouds up to the point where star formation takes place. This renders a reasonable simplification given that we consider the structure of the gas prior to stellar feedback. 3.2. Initial conditions ...
Rainbows with carbon nanotubes
... (solid lines) radial velocities of S2 star (top), as well as the corresponding O-C residuals (bottom). The left panel shows the results in the case of NTT/VLT observations and Yukawa gravity potential with Λ = 2.59· 103 AU, while the right panel shows the results for NTT/VLT+Keck combined observatio ...
... (solid lines) radial velocities of S2 star (top), as well as the corresponding O-C residuals (bottom). The left panel shows the results in the case of NTT/VLT observations and Yukawa gravity potential with Λ = 2.59· 103 AU, while the right panel shows the results for NTT/VLT+Keck combined observatio ...
![Detection of [Ne ii] Emission from Young Circumstellar Disks](http://s1.studyres.com/store/data/014394769_1-fdf9c6283148d488005c87b005dab353-300x300.png)
Detection of [Ne ii] Emission from Young Circumstellar Disks
... sky positions. These checks guarantee that the emission originates at the source location or in its proximity, within 2.00 3/pixel or ∼320 AU at a distance of 140 pc. To estimate the fluxes of the detected lines, we fit the spectrum within ±0.25 µm of each line using a Levenberg–Marquardt algorithm ...
... sky positions. These checks guarantee that the emission originates at the source location or in its proximity, within 2.00 3/pixel or ∼320 AU at a distance of 140 pc. To estimate the fluxes of the detected lines, we fit the spectrum within ±0.25 µm of each line using a Levenberg–Marquardt algorithm ...
The role of neutron star mergers in the chemical evolution of the
... Aims. We explore the problem of the production site of Eu. We also use the information present in the observed spread in the Eu abundances in the early Galaxy, and not only its average trend. Moreover, we extend our investigations to other heavy elements (Ba, Sr, Rb, Zr) to provide additional constr ...
... Aims. We explore the problem of the production site of Eu. We also use the information present in the observed spread in the Eu abundances in the early Galaxy, and not only its average trend. Moreover, we extend our investigations to other heavy elements (Ba, Sr, Rb, Zr) to provide additional constr ...
Close Double Stars from Video
... We now strongly encourage observation with relatively inexpensive video equipment to better quantify the observations, and obtain at least approximate photometric information using specially-developed software for analyzing video records, esp. Limovie from Japan and Tangra from Australia We encourag ...
... We now strongly encourage observation with relatively inexpensive video equipment to better quantify the observations, and obtain at least approximate photometric information using specially-developed software for analyzing video records, esp. Limovie from Japan and Tangra from Australia We encourag ...
Diapositiva 1
... Basic stellar parameters for single stars as input for RVS data processing: Log(g),Teff, [Fe/H], Av Derivation of L,R, age ,m using parallaxes (and stellar models) Parametrization of special sources (galaxies…) Italian contribution: Training data Galaxy simulation Cool star classification Not involv ...
... Basic stellar parameters for single stars as input for RVS data processing: Log(g),Teff, [Fe/H], Av Derivation of L,R, age ,m using parallaxes (and stellar models) Parametrization of special sources (galaxies…) Italian contribution: Training data Galaxy simulation Cool star classification Not involv ...
Diapositiva 1
... Basic stellar parameters for single stars as input for RVS data processing: Log(g),Teff, [Fe/H], Av Derivation of L,R, age ,m using parallaxes (and stellar models) Parametrization of special sources (galaxies…) ...
... Basic stellar parameters for single stars as input for RVS data processing: Log(g),Teff, [Fe/H], Av Derivation of L,R, age ,m using parallaxes (and stellar models) Parametrization of special sources (galaxies…) ...
Wroclaw_VanGrootel
... • from surface to 0.22 R* at least for sdB star Feige 48 (Porb 32 486 s) • from surface to 0.55 R* at least for sdB star PG 1336-018 (Porb 8728 s) In both cases, dynamics of deeper regions cannot be inferred with the type of pulsation modes in these short-periods sdB stars ...
... • from surface to 0.22 R* at least for sdB star Feige 48 (Porb 32 486 s) • from surface to 0.55 R* at least for sdB star PG 1336-018 (Porb 8728 s) In both cases, dynamics of deeper regions cannot be inferred with the type of pulsation modes in these short-periods sdB stars ...
Modelling galaxy spectra in presence of interstellar dust – II. From
... calculated. First, the technical details of the method are described and basic relationships/equations describing the interaction between the physical components of the galaxy are presented. Secondly, we shortly described the SSPs library in use (Piovan et al. 2003, 2006) and the space of the parame ...
... calculated. First, the technical details of the method are described and basic relationships/equations describing the interaction between the physical components of the galaxy are presented. Secondly, we shortly described the SSPs library in use (Piovan et al. 2003, 2006) and the space of the parame ...
ULX accretion states
... Two or 3 ULXs are in a weird “supersoft state”, T <~ 0.1 keV Like Galactic SS sources (= nuclear burning WDs) But can a WD reach L ~ 1E39 erg/s Photosphere of massive outflows around a BH? ...
... Two or 3 ULXs are in a weird “supersoft state”, T <~ 0.1 keV Like Galactic SS sources (= nuclear burning WDs) But can a WD reach L ~ 1E39 erg/s Photosphere of massive outflows around a BH? ...
Identification of the optical counterparts of high-mass X
... stars in the R − Hα versus B − V colour-colour diagram. We also obtained medium-resolution spectroscopy of the candidates in order to confirm the presence of Hα emission and perform spectral classification. We report on the discovery of the optical counterparts to two X-ray sources: XTE J1858+034 an ...
... stars in the R − Hα versus B − V colour-colour diagram. We also obtained medium-resolution spectroscopy of the candidates in order to confirm the presence of Hα emission and perform spectral classification. We report on the discovery of the optical counterparts to two X-ray sources: XTE J1858+034 an ...
Non-thermal hard X-ray emission from stellar coronae
... Simbol-X will allow us to explore hard-X emission from stellar coronae in a regime not reached by past observatories The best targets to search for non-thermal emission components are nearby active stars known to exhibit frequent, moderately hot flares ...
... Simbol-X will allow us to explore hard-X emission from stellar coronae in a regime not reached by past observatories The best targets to search for non-thermal emission components are nearby active stars known to exhibit frequent, moderately hot flares ...
Bamberg_VanGrootel - ORBi
... Light curve modeling + spectroscopy mass of the sdB component Need uncertainties to build a mass distribution 7 sdB stars retained in this subsample Extended sample: 15+7 22 sdB stars with accurate mass estimates • 11 (apparently) single stars • 11 in binaries (including 4 pulsators) Valerie ...
... Light curve modeling + spectroscopy mass of the sdB component Need uncertainties to build a mass distribution 7 sdB stars retained in this subsample Extended sample: 15+7 22 sdB stars with accurate mass estimates • 11 (apparently) single stars • 11 in binaries (including 4 pulsators) Valerie ...
SPY — The ESO Supernovae Type Ia Progenitor Survey
... of spectra, which have to be checked for RV variations, a fast and reliable algorithm to measure RV shifts is necessary. We apply a “cross-correlation” routine based on a χ2 test (description in Napiwotzki et al. 2001). The RV shift is evaluated from the minimum χ2. Error margins can be estimated fr ...
... of spectra, which have to be checked for RV variations, a fast and reliable algorithm to measure RV shifts is necessary. We apply a “cross-correlation” routine based on a χ2 test (description in Napiwotzki et al. 2001). The RV shift is evaluated from the minimum χ2. Error margins can be estimated fr ...
asteroseismological study of massive zz ceti stars with
... as well as oxygen–neon core white dwarf stars with stellar mass above ∼1.05 M , resulting from a progenitor star with masses between ∼7–8.5 M .6 High-mass white dwarf stars are not easy to find, not only because their intrinsically smaller number with respect to lower mass white dwarfs, but also b ...
... as well as oxygen–neon core white dwarf stars with stellar mass above ∼1.05 M , resulting from a progenitor star with masses between ∼7–8.5 M .6 High-mass white dwarf stars are not easy to find, not only because their intrinsically smaller number with respect to lower mass white dwarfs, but also b ...
When Will Mankind Achieve “First Contact” with Extraterrestrial Life
... components (i.e., light waves) from the distant objects’ light spectrums to produce a composite image that has much higher optical resolution and clarity than is possible with each individual telescope alone. This new computer assisted multiple telescope technique is referred to by scientists as int ...
... components (i.e., light waves) from the distant objects’ light spectrums to produce a composite image that has much higher optical resolution and clarity than is possible with each individual telescope alone. This new computer assisted multiple telescope technique is referred to by scientists as int ...
Constellations Overview
... The most famous of all the constellations are the 12 that make up the Zodiac. All planets can be observed only in these 12 constellations as they pass across the sky during the course of their year. This is because the orbits of all the planets lie within ± 8º of the ecliptic. The Sun also moves t ...
... The most famous of all the constellations are the 12 that make up the Zodiac. All planets can be observed only in these 12 constellations as they pass across the sky during the course of their year. This is because the orbits of all the planets lie within ± 8º of the ecliptic. The Sun also moves t ...
Superbubble Activity in Star-Forming Galaxies M. S. Oey
... compiled by Puche et al. (1992). Tongue & Westpfahl (1995) found that the SN rate implied by radio continuum emission is consistent with the hole energetics in that galaxy. However, Rhode et al. (1999) carried out a direct, BV R search for remnant stellar populations within the H i holes, and found ...
... compiled by Puche et al. (1992). Tongue & Westpfahl (1995) found that the SN rate implied by radio continuum emission is consistent with the hole energetics in that galaxy. However, Rhode et al. (1999) carried out a direct, BV R search for remnant stellar populations within the H i holes, and found ...
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.