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Booklet - Centrum Astronomiczne im. M.Kopernika PAN
... The evolutionary state of Miras with changing pulsation period S. Uttenthaler, University of Vienna, Department of Astronomy, Austria We present an investigation of the evolutionary state of Mira variables with changing pulsation period. The changing periods have been speculated to be the consequenc ...
... The evolutionary state of Miras with changing pulsation period S. Uttenthaler, University of Vienna, Department of Astronomy, Austria We present an investigation of the evolutionary state of Mira variables with changing pulsation period. The changing periods have been speculated to be the consequenc ...
... out in a single emission line, makes PNe visible out to very large distances, and makes them ideal kinematic tracers of dark matter and of abundances of stellar populations, including areas where there is little or no young stellar population. The morphologies point to the physics of the ejection pr ...
properties and evolution of disks around pre-main
... 1996). We will adopt here an “evolutionary” definition of HAeBe; namely, all stars of spectral type approximately in the range A–B that lie on PMS evolutionary tracks in the HR diagram. This criterion is applied very loosely to stars earlier than about B2, which remain on the zero-age main sequence ...
... 1996). We will adopt here an “evolutionary” definition of HAeBe; namely, all stars of spectral type approximately in the range A–B that lie on PMS evolutionary tracks in the HR diagram. This criterion is applied very loosely to stars earlier than about B2, which remain on the zero-age main sequence ...
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... cooler white dwarf sample of Bergeron, Saffer & Liebert (1992), then the hydrogen layer mass must be considerably less than 1 0 - 4 M * . In this context, Mh < 1 0 - 6 M * suffices, and this is not surprising, given that the two major channels of spectral evolution will have DA stars through the 30 ...
... cooler white dwarf sample of Bergeron, Saffer & Liebert (1992), then the hydrogen layer mass must be considerably less than 1 0 - 4 M * . In this context, Mh < 1 0 - 6 M * suffices, and this is not surprising, given that the two major channels of spectral evolution will have DA stars through the 30 ...
O stars with weak winds: the Galactic case - Max-Planck
... the stars studied here. First, the VLT archive provided UVES spectra for HD 152590, HD 38666 and HD 46202. The instrumental resolution varies between 0.04 Å and 0.1 Å, due to different slit widths. The UVES pipeline was used for the reduction of the data. Second, optical data for HD 34078 and HD 1 ...
... the stars studied here. First, the VLT archive provided UVES spectra for HD 152590, HD 38666 and HD 46202. The instrumental resolution varies between 0.04 Å and 0.1 Å, due to different slit widths. The UVES pipeline was used for the reduction of the data. Second, optical data for HD 34078 and HD 1 ...
Star formation rates and efficiencies in the Galactic Centre
... state of star formation, where the energy input from feedback (which stops gravitational collapse) is balanced by the energy dissipation (which allows gravitational collapse), cannot be reached within the Galactic Centre, again requiring some degree of episodicity. Suzuki et al. (2015) also predict ...
... state of star formation, where the energy input from feedback (which stops gravitational collapse) is balanced by the energy dissipation (which allows gravitational collapse), cannot be reached within the Galactic Centre, again requiring some degree of episodicity. Suzuki et al. (2015) also predict ...
The Formation of Massive Stars - Max-Planck
... much has been published. Some initial ideas about observational quantities at the initial stages of massive cloud collapse were discussed by Evans et al. (2002). Garay et al. (2004) presented early millimeter observations of a sample of four sources; other recent statistical identifications and stud ...
... much has been published. Some initial ideas about observational quantities at the initial stages of massive cloud collapse were discussed by Evans et al. (2002). Garay et al. (2004) presented early millimeter observations of a sample of four sources; other recent statistical identifications and stud ...
- Philsci
... A number of caveats apply, and it is best to introduce them straightaway. The case study is, of course, open to alternative interpretations. It is employed as an argument in two different senses. First, the case study exemplifies the thesis that fictional assumptions play an inferential role in mod ...
... A number of caveats apply, and it is best to introduce them straightaway. The case study is, of course, open to alternative interpretations. It is employed as an argument in two different senses. First, the case study exemplifies the thesis that fictional assumptions play an inferential role in mod ...
Kinematics of Arp 270: gas flows, nuclear activity
... Condon, Cotton & Broderick (2002). Then, using the calibration of Kennicutt et al. (2009) (equation 12) to correct for dust attenuation using 1.4 GHz luminosity, we have found that the global SFR for NGC 3396 needs to be corrected by a factor of 2.3 and NGC 3395 needs to be corrected by a factor of ...
... Condon, Cotton & Broderick (2002). Then, using the calibration of Kennicutt et al. (2009) (equation 12) to correct for dust attenuation using 1.4 GHz luminosity, we have found that the global SFR for NGC 3396 needs to be corrected by a factor of 2.3 and NGC 3395 needs to be corrected by a factor of ...
Determination of the position angle of stellar spin axes
... determine the stellar position angle directly within 10◦ with a signal-to-noise ratio of the order of 6. Under less favourable conditions, i.e. larger plate scale or smaller stellar diameter, the cross-correlation method yields comparable results. Conclusions. We show that with the currently existin ...
... determine the stellar position angle directly within 10◦ with a signal-to-noise ratio of the order of 6. Under less favourable conditions, i.e. larger plate scale or smaller stellar diameter, the cross-correlation method yields comparable results. Conclusions. We show that with the currently existin ...
Jaká kritéria jsou vhodná ke klasifikaci hvězd horní části hlavní
... Spectroscopy today is a highly developed method of studying electromagnetic radiation and stands as method bringing a vast amount of information about distant objects to us. Product of a spectroscopic measurement is called a spectrum and it is essentially a function of distribution of radiation resp ...
... Spectroscopy today is a highly developed method of studying electromagnetic radiation and stands as method bringing a vast amount of information about distant objects to us. Product of a spectroscopic measurement is called a spectrum and it is essentially a function of distribution of radiation resp ...
Stellar interactions in dense and sparse star clusters
... Context. Stellar encounters potentially affect the evolution of the protoplanetary discs in the Orion Nebula Cluster (ONC). However, the role of encounters in other cluster environments is less known. Aims. We investigate the effect of the encounter-induced disc-mass loss in different cluster environme ...
... Context. Stellar encounters potentially affect the evolution of the protoplanetary discs in the Orion Nebula Cluster (ONC). However, the role of encounters in other cluster environments is less known. Aims. We investigate the effect of the encounter-induced disc-mass loss in different cluster environme ...
The Occurrence Rate of Small Planets Around Small Stars
... We assign revised stellar parameters by comparing the observed optical and near infrared colors of all 51813 cool (TKIC ≤ 5050K) and all 13402 unclassified Kepler planet search target stars to the colors of model stars. We account for interstellar reddening by determining the distance at which the a ...
... We assign revised stellar parameters by comparing the observed optical and near infrared colors of all 51813 cool (TKIC ≤ 5050K) and all 13402 unclassified Kepler planet search target stars to the colors of model stars. We account for interstellar reddening by determining the distance at which the a ...
Rapid Rotation of Low-Mass Red Giants Using APOKASC: A
... able to measure line broadenings below 5 km s−1 , reduced χ2 values indicate that our results begin to differ from published results below this value; thus our measurements below 5 km s−1 should be considered nondetections. Above this value, our results are consistent with the Molenda-Żakowicz resu ...
... able to measure line broadenings below 5 km s−1 , reduced χ2 values indicate that our results begin to differ from published results below this value; thus our measurements below 5 km s−1 should be considered nondetections. Above this value, our results are consistent with the Molenda-Żakowicz resu ...
Numerical Star-Formation Studies-
... density of gravitational stability. These clumps begin to collapse, their central density increases rapidly, and eventually they give birth to new protostars. Clusters of stars form in large regions that become unstable, within which contraction involves multiple collapsing cloud cores. A number of ...
... density of gravitational stability. These clumps begin to collapse, their central density increases rapidly, and eventually they give birth to new protostars. Clusters of stars form in large regions that become unstable, within which contraction involves multiple collapsing cloud cores. A number of ...
REVIEW Numerical Star-Formation Studies— A Status Report
... problem into smaller bits and pieces and by focusing on few feedback loops. Stars of all ages radiate and will thus heat up physical processes or single scales only. Today, however, algothe gas in their vicinity. By doing so they influence subsequent rithmic advances and increasing computational powe ...
... problem into smaller bits and pieces and by focusing on few feedback loops. Stars of all ages radiate and will thus heat up physical processes or single scales only. Today, however, algothe gas in their vicinity. By doing so they influence subsequent rithmic advances and increasing computational powe ...
Astronomy Astrophysics - Max Planck Institut für Radioastronomie
... 1. Introduction Accretion disks around young stellar objects (YSOs) are at the focus of astronomical research, not only because they play an essential role in the star-formation process, but also because they provide the stage where planet formation takes place. Historically, these disks were discov ...
... 1. Introduction Accretion disks around young stellar objects (YSOs) are at the focus of astronomical research, not only because they play an essential role in the star-formation process, but also because they provide the stage where planet formation takes place. Historically, these disks were discov ...
How Massive Single Stars End Their Life - TigerPrints
... by the mass of the helium core when the star dies. (Perhaps the carbon oxygen core mass is a better discriminant, but systematics of the two are very similar.) As the mass of the helium core increases, so does its binding energy and entropy. Because of its higher entropy, a larger helium core also h ...
... by the mass of the helium core when the star dies. (Perhaps the carbon oxygen core mass is a better discriminant, but systematics of the two are very similar.) As the mass of the helium core increases, so does its binding energy and entropy. Because of its higher entropy, a larger helium core also h ...
The effects of red supergiant mass loss on
... lower than the escape velocity from the stellar photosphere, v esc ∼ 100 km s−1 . He assessed the possibility that radiation pressure on the circumstellar ions (and atoms) could drive the wind until the local escape velocity would have dropped below the wind speed, but the values for the achieved ac ...
... lower than the escape velocity from the stellar photosphere, v esc ∼ 100 km s−1 . He assessed the possibility that radiation pressure on the circumstellar ions (and atoms) could drive the wind until the local escape velocity would have dropped below the wind speed, but the values for the achieved ac ...
Large distance of epsilon Aurigae from interstellar
... that our EWs only represent a lower limit to the true EW of the 6613 DIB but in the light of the above-mentioned studies we do believe that with a homogeneous series of the spectra taken with the same instrument a calibration of the 6613 DIB vs. distance within a limited area in the sky should be fe ...
... that our EWs only represent a lower limit to the true EW of the 6613 DIB but in the light of the above-mentioned studies we do believe that with a homogeneous series of the spectra taken with the same instrument a calibration of the 6613 DIB vs. distance within a limited area in the sky should be fe ...
the mass-loss return from evolved stars to the large
... SSTSAGE052206 occupies region F, identified by Nikolaev & Weinberg (2000) as O-rich AGB stars of intermediate age. The other star, HV 5715, was located in region G of the 2MASS CMD plotted by Nikolaev & Weinberg (2000), corresponding to young AGB stars that have such a high mass that hot-bottom burn ...
... SSTSAGE052206 occupies region F, identified by Nikolaev & Weinberg (2000) as O-rich AGB stars of intermediate age. The other star, HV 5715, was located in region G of the 2MASS CMD plotted by Nikolaev & Weinberg (2000), corresponding to young AGB stars that have such a high mass that hot-bottom burn ...
the red supergiant content of m31
... stars lose most of their hydrogen-rich envelopes and exploded instead as type II-L or even type Ib supernovae. The validity of this resolution rests on the assumption that the RSG mass-loss rates have been seriously underestimated. Meynet et al. (2015) and Georgy et al. (2015) proposed a novel way o ...
... stars lose most of their hydrogen-rich envelopes and exploded instead as type II-L or even type Ib supernovae. The validity of this resolution rests on the assumption that the RSG mass-loss rates have been seriously underestimated. Meynet et al. (2015) and Georgy et al. (2015) proposed a novel way o ...
Large-eddy simulations of isolated disc galaxies with thermal and
... Miura et al. 2012) before they are destroyed by supernova explosions (SNe) and stellar winds. Actively star-forming molecular clouds are known to be strongly supersonically turbulent with typical velocity dispersions around 10 km s−1 (e.g. Leroy et al. 2008; Stilp et al. 2013), or larger in interact ...
... Miura et al. 2012) before they are destroyed by supernova explosions (SNe) and stellar winds. Actively star-forming molecular clouds are known to be strongly supersonically turbulent with typical velocity dispersions around 10 km s−1 (e.g. Leroy et al. 2008; Stilp et al. 2013), or larger in interact ...
Does feedback help or hinder star formation? The effect of
... assumes solar metallicity and a Salpeter initial mass function between 1 − 100 M⊙ . Within this range, the IMF gradient does not depend strongly on model choice, for example giving a similar distribution to the Chabrier IMF (Chabrier 2005). The rays are assumed to be monochromatic with the mean ioni ...
... assumes solar metallicity and a Salpeter initial mass function between 1 − 100 M⊙ . Within this range, the IMF gradient does not depend strongly on model choice, for example giving a similar distribution to the Chabrier IMF (Chabrier 2005). The rays are assumed to be monochromatic with the mean ioni ...
Gas giants in hot water: inhibiting giant planet
... I show that in the interior of massive embedded star clusters, the temperature approaches and exceeds the condensation temperature of water ice, TIce 150–170 K (Podolak & Zucker 2004; Lecar et al. 2006). Because the discs equilibrate to midplane temperatures at or above the value corresponding to ...
... I show that in the interior of massive embedded star clusters, the temperature approaches and exceeds the condensation temperature of water ice, TIce 150–170 K (Podolak & Zucker 2004; Lecar et al. 2006). Because the discs equilibrate to midplane temperatures at or above the value corresponding to ...