Relevant bibliographies by topics / AGB stars

Contents

  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'AGB stars'

Author: Grafiati
Published: 4 June 2021
Last updated: 9 March 2023

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Journal articles on the topic "AGB stars"

1

Suh, Kyung-Won. "Infrared studies of post-AGB stars and PNe." Proceedings of the International Astronomical Union 12, S323 (October 2016): 28–31. http://dx.doi.org/10.1017/s1743921317002204.

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AbstractWe present infrared two color diagrams (2CDs) for a large sample of AGB stars, post-AGB stars, and planetary nebulae (PNe) to study their spectral evolution in infrared bands. We discuss possible evolutionary tracks from AGB stars to PNe on the 2CDs. We use catalogs from the available literature for the sample of AGB stars, post-AGB stars, and PNe in our Galaxy.
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Sargent, B., S. Srinivasan, M. Boyer, M. Feast, P. Whitelock, M. Marengo, M. A. T. Groenewegen, M. Meixner, J. L. Hora, and M. Otsuka. "Infrared Studies of the Variability and Mass Loss of Some of the Dustiest Asymptotic Giant Branch Stars in the Magellanic Clouds." Proceedings of the International Astronomical Union 14, S343 (August 2018): 498–99. http://dx.doi.org/10.1017/s1743921318007068.

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AbstractThe asymptotic giant branch (AGB) stars with the reddest colors have the largest amounts of circumstellar dust. AGB stars vary in their brightness, and studies show that the reddest AGB stars tend to have longer periods than other AGB stars and are more likely to be fundamental mode pulsators than other AGB stars. Such stars are difficult to study, as they are often not detected at optical wavelengths. Therefore, they must be observed at infrared wavelengths. Using the Spitzer Space Telescope, we have observed a sample of very dusty AGB stars in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) over Cycles 9 through 12 during the Warm Spitzer mission. For each cycle’s program, we typically observed a set of AGB stars at both 3.6 and 4.5 μm wavelength approximately monthly for most of a year. We present results from our analysis of the data from these programs.
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Parthasarathy, M. "Evolutionary connection between C-rich AGB stars and C-rich central stars of PNe." Symposium - International Astronomical Union 191 (1999): 475–80. http://dx.doi.org/10.1017/s0074180900203434.

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On the basis of C/O ratios the evolutionary connection between C-rich AGB/post-AGB stars and C-rich central stars of PNe is discussed. The proportion of carbon-rich post-AGB stars is comparable to that of carbon-rich PNe. The post-AGB stars with 21μm emission are found to be over abundant in carbon and s-process elements indicating that they have gone through the third dredge-up and carbon star phase on the AGB. As these stars evolve to higher temperature they will form carbon-rich PNe with carbon-rich central stars. Analysis of C/O ratios of PNe suggests that 68 percent of PNe have C/O > 1 indicating that the progenitors have gone through the third dredge-up and carbon-rich phase on the AGB. The Type I PNe can be divided into two groups. Group I Type I PNe are those with C/O < 1 indicating that their massive progenitors have gone through the third dredge-up and hot bottom burning on the AGB. Group II Type I PNe are those with C/O > 1. Their progenitors have gone through third dredge-up only and may not have experienced hot bottom burning. Carbon stars with silicate dust and or carbon-rich post-AGB stars (such as post-AGB stars with 21μm emission) may be the progenitors of PNe with [WC] central stars. The evolutionary sequence seems to be: carbon-rich AGB → carbon-rich post-AGB → [WC late type] → [WC early type] → [WC-PG 1159] → PG 1159.
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Kamath, Devika, and Hans Van Winckel. "Post-AGB Stars as Tracers of AGB Nucleosynthesis: An Update." Universe 8, no. 4 (April 11, 2022): 233. http://dx.doi.org/10.3390/universe8040233.

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The chemical evolution of galaxies is governed by the chemical yields from stars, and here we focus on the important contributions from asymptotic giant branch (AGB) stars. AGB nucleosynthesis is, however, still riddled with complexities. Observations from post-asymptotic giant branch (post-AGB) stars serve as exquisite tools to quantify and understand AGB nucleosynthesis. In this contribution, we review the invaluable constraints provided by post-AGB stars with which to study AGB nucleosynthesis, especially the slow neutron capture nucleosynthesis (i.e., the s-process).
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Parthasarathy, M., Marina Kounkel, and Keivan G. Stassun. "Evolutionary Status of Selected Post-AGB Single and Binary Stars in Gaia DR3." Research Notes of the AAS 6, no. 8 (August 26, 2022): 171. http://dx.doi.org/10.3847/2515-5172/ac8c46.

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Abstract Gaia data is helping to further understand the evolutionary status of post-AGB and related stars. In this paper we present an analysis of Gaia DR3 data of post-AGB stars and post-AGB binaries with accurate parallaxes. Gaia DR3 data of 44 post-AGB candidates are analyzed, including 16 post-AGB binary candidates. Of these, 19 stars have RUWE values >1.4. For several stars, the calculated absolute luminosities confirm that they are indeed in post-AGB evolutionary stage. We find that 12 stars have relatively lower luminosities; some of them may be post-RGB stars and some may be post-HB stars. We find that IRAS 01427+4633 (BD+46 442), IRAS 16230–3410, and IRAS 19199+3950 (HP Lyr) are evolved high velocity stars.
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Saberi, Maryam. "Tracing the role of AGB stars in the Galactic Fluorine budget." Proceedings of the International Astronomical Union 16, S366 (November 2020): 196–98. http://dx.doi.org/10.1017/s1743921322000412.

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AbstractThe cosmic origin of fluorine is still under debate. Asymptotic giant branch (AGB) stars are among the few suggested candidates to efficiently synthesis F in our Galaxy, however their relative contribution is not clear. In this paper, we briefly review the theoretical studies from stellar yield models of the F synthesis and chemical equilibrium models of the F-containing molecules in the outflow around AGB stars. Previous detections of the F-bearing species towards AGB and post-AGB stars are also highlighted. We suggest that high-resolution ALMA observations of the AlF, one of the two main carriers of F in the outflow of AGB stars, can provide a reliable tracer of the F-budget in AGB stars. This will be helpful to quantify the role of AGB stars in the Galactic F budget.
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Loup, C., E. Josselin, M. R. Cioni, H. J. Habing, J. A. D. L. Blommaert, N. R. Trams, M. A. T. Groenewegen, et al. "ISOCAM and DENIS Survey of 0.5 square degrees in the Bar of the LMC. Detection of the whole TP-AGB Star Population." Symposium - International Astronomical Union 191 (1999): 561–66. http://dx.doi.org/10.1017/s0074180900203550.

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We surveyed 0.5 square degrees in the Bar of the LMC with ISOCAM at 4.5 and 12 μm, and with DENIS in the I, J, and Ks bands. Our goal was to build a complete sample of Thermally-Pulsing AGB stars. Here we present the first analysis of 0.14 square degrees. In total we find about 300 TP-AGB stars. Among these TP-AGB stars, 9% are obscured AGB stars (high mass-loss rates); 9 of them were detected by IRAS, and only 1 was previously identified. Their luminosities range from 2 500 to 14 000 L⊙, with a distribution very similar to the one of optical TP-AGB stars (i.e. those with low mass-loss rates). Such a luminosity distribution, as well as the percentage of obscured stars among TP-AGB stars, is in very good agreement with the evolutionary models of Vassiliadis & Wood (1993) if most of the TP-AGB stars that we find have initial masses smaller than 1.5 to 2 M⊙.
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Waters, L. B. F. M., C. Waelkens, and H. Van Winckel. "Binary post-AGB stars." Symposium - International Astronomical Union 180 (1997): 313–18. http://dx.doi.org/10.1017/s0074180900131146.

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Low and intermediate mass stars leave the Asymptotic Giant Branch (AGB) when the mass in their H-rich envelope is less than about 0.01 M⊙, and the high mass loss drops several orders of magnitude. The central star rapidly evolves to the left part of the HR diagram along a track of constant luminosity (e.g. Schönberner 1983). In principle the evolution of the central star to higher Teff and the expansion and cooling of the AGB remnant are easy to calculate. In practice several complicating factors arise which make it much more difficult to predict the morphology and properties of post-AGB stars, such as binarity, post-AGB mass loss and aspherical AGB mass loss. Binarity of post-AGB stars affects the morphology of the circumstellar environment, and it affects evolutionary timescales and surface chemical abundances of the components in the system. This review discusses some properties of binary post-AGB stars.
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Frantsman, Yu L. "The Ratio of the Numbers of Carbon Stars to M Stars in Galaxies." International Astronomical Union Colloquium 106 (1989): 51. http://dx.doi.org/10.1017/s0252921100062606.

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Simulated populations of the AGB stars were calculated with different assumptions about mass loss, initial chemical composition and dredge-up efficiency. The early-AGB (E-AGB) phase was taken into account. The numbers of carbon and oxygen stars per 106 generated stars and the ratio (NC/NM) of these numbers were obtained. It is possible to match theoretically obtained NC/NM with the observations only if the luminosity of observed stars Mbol < -3.5; otherwise it is necessary to take into account the E-AGB phase. The data in the Table are for all AGB stars in the Galaxy and for stars with Mbol < -1.80 in the LMC.
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Parthasarathy, M. "Chemical Composition and Evolution of Post-AGB Stars." Symposium - International Astronomical Union 177 (2000): 225–36. http://dx.doi.org/10.1017/s0074180900002448.

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Analysis of the chemical compositions of post-AGB stars reveals the following abundance patterns: (i) Post-AGB stars which are extremely underabundant in Fe and other refractory elements, but which have nearly normal abundances of C, N, O, S, and Zn. The depleted refractory elements are locked up in circumstellar dust grains. Formation of dust close to the star, and dust-gas separation and dust-driven mass loss driving out mostly the dust may explain the abundances of these stars. (ii) High-latitude hot post-AGB stars which show an underabundance of carbon, indicating that they left the AGB before the third dredge-up occurred. (iii) Post-AGB stars with overabundances of carbon and s-process elements, indicating that they have gone through the third dredge-up and carbon-star phase on the AGB. The overabundance of Li, Al, C and s-process elements in some post-AGB stars indicate that they have gone through the dredge-up and Hot Bottom Burning nucleosynthesis at the base of the convective envelope. The observed characteristics of post-AGB stars indicate an evolutionary sequence in the transition region from the tip of the AGB into the young planetary nebula stage.
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Dissertations / Theses on the topic "AGB stars"

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Siderud, Emelie. "Dust emission modelling of AGB stars." Thesis, Uppsala universitet, Observationell astrofysik, 2020. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-423949.

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Groenewegen, Martin Arnold Theodoor. "On the evolution and properties of AGB stars." Amsterdam : Amsterdam : Sterrenkundig Instituut 'Anton Pannekoek' ; Universiteit van Amsterdam [Host], 1993. http://dare.uva.nl/document/91969.

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Lau, Ho Bun. "Evolution and nucleosynthesis of zero-metallicity AGB stars." Thesis, University of Cambridge, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.612023.

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Bladh, Sara. "Dynamical atmospheres and winds of M-type AGB stars." Doctoral thesis, Uppsala universitet, Institutionen för fysik och astronomi, 2014. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-230645.

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Mass loss, in the form of slow stellar winds, is a decisive factor for the evolution of cool luminous giants, eventually turning them into white dwarfs. These dense outflows are also a key factor in the enrichment of the interstellar medium with newly produced elements from the interior of these stars. There are strong indications that these winds are accelerated by radiation pressure on dust grains, but the actual grain species responsible for driving the outflows in M-type Asymptotic Giant Branch stars are still a matter of debate. Observations of dust features in the circumstellar environment of these stars suggest that magnesium-iron silicates are possible wind-drivers. However, the optical properties of these silicate grains are strongly influenced by the Fe-content. Fe-bearing condensates heat up strongly when interacting with the radiation field and therefore cannot form close enough to the star to trigger outflows. Fe-free condensates, on the other hand, have a low absorption cross-section at near-IR wavelengths where AGB stars emit most of their flux.  To solve this conundrum, it has been suggested that winds of M-type AGB stars may be driven by photon scattering on Fe-free silicate grains with sizes comparable to the wavelength of the flux maximum, rather than by true absorption. In this thesis we investigate dynamical models of M-type AGB stars, using Fe-free silicates as the wind-driving dust species. According to our findings these models produce both dynamic and photometric properties consistent with observations. Especially noteworthy are the large photometric variations in the visual band during a pulsation cycle, seen both in the observed and synthetic fluxes. A closer examination of the models reveals that these variations are caused by changes in the molecular layers, and not by changes in the dust. This is a strong indication that stellar winds of M-type AGB stars are driven by dust materials that are very transparent in the visual and near-infrared wavelength regions, otherwise these molecular effects would not be visible.
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Weston, Simon. "Post asymptotic giant branch and central stars of planetary nebulae in the Galactic halo." Thesis, University of Hertfordshire, 2012. http://hdl.handle.net/2299/9042.

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Post asymptotic giant branch (post-AGB) stars, central stars of planetary nebulae (CSPNe) and planetary nebulae (PNe) are important phases of stellar evolution as the material they feedback is the seed of subsequent star formation in a galaxy. The majority of low and intermediate mass stars are expected to evolve through these channels, however, it is uncertain how many actually do, and at what rate. The Galactic halo, with its older population, provides a direct test of evolutionary models for low mass stars. Birthrate estimates of PNe are uncertain and worse still, are in contradiction with accepted white dwarf (WD) birthrate estimates. Much of the uncertainty stems from the lack of complete samples and poorly determined distance estimates. New surveys such as the Sloan Digital Sky Survey (SDSS), Galaxy Evolutionary Ex- plorer (GALEX) and the INT Photometric H® Survey (IPHAS) have discovered many new PNe and have observed the far edges of the Galaxy. Improved methods of determining distances to CSPNe are presented here, using model atmospheres, evolutionary tracks and high resolution reddening maps utilising these revolution- ary surveys. Locating the CSPN is non-trivial particularly for evolved PNe, as they are ex- tended with their central star often displaced from the centre of the nebula. There- fore, photometric criteria are required to locate the CSPN in the nebula’s field. Synthetic photometry of the CSPNe is derived from spectral energy distributions (SEDs) computed from a grid of model atmospheres covering the parameter range of CSPNe. The SEDs are convolved with filter transmission curves to compute synthetic magnitudes for a given photometric system which are then calibrated with standard stars and WDs. A further project borne out of a search for luminous central stars of faint PNe, resulted in a systematic search for post-AGB stars in the Galactic halo. In this work, new candidate halo post-AGB stars are discovered from a search through the SDSS spectroscopic database. Combined with previously identified halo post- AGB stars, including the results of a sub-sample from the Palomar-Green (PG) survey, the number of observed and predicted populations are compared. The number of observed post-AGB candidates shows a remarkable deficit to expecta- tions. A survey within a subset of the photometric database of SDSS supports the findings of the PG and SDSS spectroscopic surveys. These findings provide strong evidence for a lack of post-AGB stars in the Galac- tic halo and thick disc. A plausible explanation is that a large fraction of stars in these old, metal-poor populations are evolving via alternative channels. The implications of such a result are far reaching with knock on effects for stellar evolutionary theory, galactic evolution and extragalactic redshift estimates.
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Brogan, Roisin. "The Variability of the R Magnitude in Dynamical Models of AGB Stars." Thesis, Uppsala universitet, Teoretisk astrofysik, 2019. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-392377.

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This report will first give a brief background on asymptotic giant branch (AGB) stars and the characteristics that make them interesting to study. Some methods and tools used in the field are then introduced, before the photometric variability of these stars is investigated. This is achieved by using data from dynamical models of AGB stars with differing chemical abundances. The R, J and K bands of the UBVRI system are specifcally investigated to explore whether these are good candidates for AGB photometric and spectroscopic research. Lastly, the molecular features at these wavelengths are investigated to understand the impact that they have on the photometric variability during the pulsation cycle and which molecules are most prominent in this.
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Ireland, Michael James. "Optical Interferometry and Mira Variable Stars." Thesis, The University of Sydney, 2005. http://hdl.handle.net/2123/721.

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This thesis describes the development of a red tip/tilt and fringe detection system at the Sydney University Stellar Interferometer (SUSI), modelling the instrumental performance and effects of seeing at SUSI, making observations of Mira variable stars and finally modelling the atmospheres of Mira variables with physically self-consistent models. The new SUSI tip/tilt system is based around a CCD detector and has been successfully used to both track the majority of tip/tilt power in median seeing at an R magnitude of 4.5, and to provide seeing measures for post processing. The new fringe-detection system rapidly scans 33 to 140 $\mu$m in delay and detects the fringes using two avalanche-photodiodes. It has been used to acquire fringe data, provide user feedback and to track the fringe group-delay position. The system visibility (fringe visibility for a point source) and throughput were found to be consistent with models of the SUSI optical beam train. Observations were made of a variety of sources, including the Mira variables R Car and RR Sco, which were observed in two orthogonal polarization states. These measurements were the first successful use of Optical Interferometric Polarimetry (OIP), and enabled scattered light to be separated from bright photospheric flux. Dust scattering was found to originate from a thin shell 2-3 continuum radii from these stars, with an optical depth of 0.1 to 0.2 at 900 nm. Physical models of Mira variables including dust formation were developed, providing consistent explanations for these results as well as many other photometric and interferometric observations.
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Ireland, Michael James. "Optical Interferometry and Mira Variable Stars." University of Sydney. Physics, 2005. http://hdl.handle.net/2123/721.

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This thesis describes the development of a red tip/tilt and fringe detection system at the Sydney University Stellar Interferometer (SUSI), modelling the instrumental performance and effects of seeing at SUSI, making observations of Mira variable stars and finally modelling the atmospheres of Mira variables with physically self-consistent models. The new SUSI tip/tilt system is based around a CCD detector and has been successfully used to both track the majority of tip/tilt power in median seeing at an R magnitude of 4.5, and to provide seeing measures for post processing. The new fringe-detection system rapidly scans 33 to 140 $\mu$m in delay and detects the fringes using two avalanche-photodiodes. It has been used to acquire fringe data, provide user feedback and to track the fringe group-delay position. The system visibility (fringe visibility for a point source) and throughput were found to be consistent with models of the SUSI optical beam train. Observations were made of a variety of sources, including the Mira variables R Car and RR Sco, which were observed in two orthogonal polarization states. These measurements were the first successful use of Optical Interferometric Polarimetry (OIP), and enabled scattered light to be separated from bright photospheric flux. Dust scattering was found to originate from a thin shell 2-3 continuum radii from these stars, with an optical depth of 0.1 to 0.2 at 900 nm. Physical models of Mira variables including dust formation were developed, providing consistent explanations for these results as well as many other photometric and interferometric observations.
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Lam, Doan Duc. "The circumstellar envelope of the S-type AGB star π1 Gruis." Licentiate thesis, Uppsala universitet, Teoretisk astrofysik, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-327397.

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Lykou, Foteini. "Dusty discs around evolved stars." Thesis, University of Manchester, 2013. https://www.research.manchester.ac.uk/portal/en/theses/dusty-discs-around-evolved-stars(eecbf437-9e03-4bf5-b4ee-77a831c9b017).html.

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From the main sequence onwards, stars of intermediate masses (1-8 Solar masses) eject a large portion of their mass with rates as high as 0.0001 Solar masses per year during their transition through the Asymptotical Giant Branch (AGB) stage. The outflows are shaped by the same mechanisms that shape the ejecta, which in turn appear to depart from spherical symmetry as early as the AGB stage. The ejecta are then evolving into asymmetrical structures. Stars like that are giant factories of dust, responsible for the enrichment of their surrounding Galactic medium in metals heavier than helium. Depending on their abundances during the AGB stage, the stars are either oxygen-rich or carbon-rich, and as such, the dust produced in their atmospheres is either O-rich or C-rich. The chemical composition of the ejecta, indicates the stellar chemistry at the moment of ejection. The disruption of the spherical symmetry of the mass loss can be caused by fast rotation, stellar magnetic fields or binarity, the latter being the most efficient and favourable mechanism. Such mechanisms can lead to the creation of circumstellar, equatorial, dusty structures, like discs, torii or spirals. Due to their small relative sizes, compared to their surrounding nebulae, they can be studied at best with the use of infrared interferometric techniques. We report the discovery of three such structures in sources at three different evolutionary stages, respectively, with the use of single- and multi-aperture interferometry. In the C-rich AGB star V Hya we imaged via aperture masking in the near-infrared, a complex and possibly orbiting structure, which is embedded within the star's molecular torus. Our MIDI observations in the mid-infrared have revealed, a silicate disc within the symbiotic nebula M2-9 that is currently being shaped by the central binary system within its core, and a C-rich disc-like structure in the born-again star Sakurai's Object, that is also aligned to an asymmetry found in its surrounding planetary nebula. Finally, we compare the properties of the structures found here with those found in the literature in order to establish a relation between late stellar evolution and the existence of dusty structures.
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Books on the topic "AGB stars"

1

R, Szczerba, and Górny S. K, eds. Post-AGB objects as a phase of stellar evolution: Proceedings of the Toruń workshop held July 5-7, 2000. Dordrecht: Kluwer Academic Publishers, 2001.

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F, Kerschbaum, Charbonnel Corinne, and Wing Robert F, eds. Why galaxies care about AGB stars: Their importance as actors and probes : proceedings of an international conference held at University Campus, Vienna, Austria, 7-11 August, 2006. San Francisco, Calif: Astronomical Society of the Pacific, 2007.

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ESO/CTIO, Workshop on Mass Loss on the AGB and Beyond (2nd 1992 La Serena Chile). Second ESO/CTIO Workshop on Mass Loss on the AGB and Beyond: La Serena, Chile, 21-24 January 1992 : proceedings. Garching bei München: ESO, 1993.

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Kerschbaum, F. Why galaxies care about AGB stars II: Shining examples and common inhabitants : proceedings of a conference held at University Campus, Vienna, Austria, 16-20 August 2010. Edited by Astronomical Society of the Pacific. San Francisco: Astronomical Society of the Pacific, 2011.

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Roald, Guandalini, Palmerini Sara, Busso Maurizio, American Institute of Physics, Università di Perugia, and Perugia Workshop on Nuclear Astrophysics (2nd : 2007 : Perugia, Italy), eds. The Ninth Torino Workshop on evolution and nucleosynthesis in AGB stars and the Second Perugia Workshop on Nuclear Astrophysics: Held in Perugia, Italy, 21-27 October 2007. [Melville, N.Y.]: American Institute of Physics, 2008.

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E, Mamajek Eric, Soderblom David R, and Wyse Rosemary F. G, eds. The ages of stars: Proceedings of the 258th Symposium of the International Astronomical Union held in Baltimore, Maryland, USA, October 13-17, 2008. Cambridge: Cambridge University Press, 2009.

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Sandage, Allan. The age of the galactic disk. Baltimore, MD: Space Telescope Science Institute, 1990.

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Mattison, Alice. Field of stars. New York: Morrow, 1992.

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O'Connor, Sheila. Keeping safe the Stars. New York: G. P. Putnam's Sons, 2012.

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Puttock, Simon. A ladder to the stars. London: Frances Lincoln, 2002.

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Book chapters on the topic "AGB stars"

1

Waelkens, Christoffel, and Rens B. F. M. Waters. "Post-AGB Stars." In Astronomy and Astrophysics Library, 519–53. New York, NY: Springer New York, 2004. http://dx.doi.org/10.1007/978-1-4757-3876-6_10.

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Waters, L. B. F. M., C. Waelkens, and H. Van Winckel. "Binary Post-Agb Stars." In Planetary Nebulae, 313–18. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5244-0_150.

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Gustafsson, Bengt, and Susanne Höfner. "Atmospheres of AGB Stars." In Astronomy and Astrophysics Library, 149–245. New York, NY: Springer New York, 2004. http://dx.doi.org/10.1007/978-1-4757-3876-6_4.

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Parthasarathy, M., G. Gauba, T. Fujii, and Y. Nakada. "Hot Post-AGB Stars." In Post-AGB Objects as a Phase of Stellar Evolution, 29–40. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-015-9688-6_4.

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Habing, Harm. "AGB and POST-AGB STARS: an Overview." In Science with the VLT Interferometer, 183–91. Berlin, Heidelberg: Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-540-69398-7_23.

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Kwok, Sun, Kate Y. L. Su, and J. A. Stoesz. "Circumstellar Arcs in AGB Post-AGB Stars." In Post-AGB Objects as a Phase of Stellar Evolution, 115–20. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-015-9688-6_17.

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Le Bertre, T., N. Epchtein, F. Guglielmo, and P. Le Sidaner. "Infrared Photometry of AGB Stars." In Science with Astronomical Near-Infrared Sky Surveys, 105–16. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0946-8_23.

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Sackmann, I. Juliana, and Arnold I. Boothroyd. "On Low Mass AGB Stars." In Evolution of Stars: The Photospheric Abundance Connection, 275–85. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3416-3_24.

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Aringer, B., F. Kerschbaum, and J. Hron. "Dust Emission from AGB Stars." In Astrophysics and Space Science, 445–46. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-5076-7_74.

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Guélin, M., R. Lucas, and R. Neri. "Mass Loss in AGB Stars." In CO: Twenty-Five Years of Millimeter-Wave Spectroscopy, 359–66. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5414-7_64.

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Conference papers on the topic "AGB stars"

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de Laverny, Patrick, and Bruno Lopez. "AGB and post-AGB stars as VLTI targets." In Astronomical Telescopes and Instrumentation, edited by Pierre J. Lena and Andreas Quirrenbach. SPIE, 2000. http://dx.doi.org/10.1117/12.390210.

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Bisterzo, S., R. Gallino, O. Straniero, I. I. Ivans, G. W. Preston, and W. Aoki. "CEMP–s Stars: AGB Yield Predictions and Thermohaline Mixing." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905573.

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Busso, M., O. Trippella, E. Maiorca, and S. Palmerini. "AGB stars & presolar grains." In SEVENTH EUROPEAN SUMMER SCHOOL ON EXPERIMENTAL NUCLEAR ASTROPHYSICS: Proceedings of the 7th European Summer School on Experimental Nuclear Astrophysics. AIP Publishing LLC, 2014. http://dx.doi.org/10.1063/1.4875288.

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Marigo, Paola. "Nucleosynthesis in TP-AGB stars." In The 3rd international symposium on nuclear astrophysics: Nuclei in the Cosmos III. AIP, 1995. http://dx.doi.org/10.1063/1.47325.

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Tsalmantza, P. "AGB stars in nearby galaxies." In RECENT ADVANCES IN ASTRONOMY AND ASTROPHYSICS: 7th International Conference of the Hellenic Astronomical Society. AIP, 2006. http://dx.doi.org/10.1063/1.2348026.

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Marengo, Massimo, Megan Reiter, Giovanni G. Fazio, Roald Guandalini, Sara Palmerini, and Maurizio Busso. "Spitzer'IRAC Observations of AGB Stars." In IXTH TORINO WORKSHOP ON EVOLUTION AND NUCLEOSYNTHESIS IN AGB STARS AND THE IIND PERUGIA WORKSHOP ON NUCLEAR ASTROPHYSICS. AIP, 2008. http://dx.doi.org/10.1063/1.2916982.

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Herwig, Falk. "AGB stars evolution & nucleosynthesis." In International Symposium on Nuclear Astrophysics - Nuclei in the Cosmos - IX. Trieste, Italy: Sissa Medialab, 2010. http://dx.doi.org/10.22323/1.028.0206.

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Husti, L., R. Gallino, and O. Straniero. "Barium Stars—AGB Predictions Confronted with Observations: a Link with CEMP‐s Stars." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905528.

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Di Criscienzo, Marcella, Paolo Ventura, and Flavia Dell’Agli. "Dust and Gas from AGB Stars." In Proceedings of the 15th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG15). Journal of the Physical Society of Japan, 2020. http://dx.doi.org/10.7566/jpscp.31.011061.

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Gallino, Roberto, Maurizio Busso, and Maria Lugaro. "Neutron capture nucleosynthesis in AGB stars." In ASTROPHYSICAL IMPLICATIONS OF THE LABORATORY STUDY OF PRESOLAR MATERIALS. ASCE, 1997. http://dx.doi.org/10.1063/1.53327.

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Reports on the topic "AGB stars"

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Götz, Konrad, Ueli Haefeli, and Daniel Meierhans. Thematische Synthese «Mobilitätsverhalten» des NFP «Energie». Swiss National Science Foundation (SNSF), September 2019. http://dx.doi.org/10.46446/publikation_nfp70_nfp71.2019.5.de.

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Wie kann der hohe Anteil des Verkehrs am Schweizer Energieverbrauch so stark reduziert werden, wie dies für die Transformation des Energiesystems nötig ist? Die Synthese leitet aus den mobilitätsbezogenen Ergebnissen des NFP Energie die zentralen Herausforderungen ab und verdichtet sie zu Handlungsempfehlungen.
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Altantuya, Jigjidsuren,, Oyun Bayar, and Habib Najibullah. Rationalizing Mongolia’s Hospital Services: Experiences, Lessons Learned, and Future Directions. Asian Development Bank, August 2021. http://dx.doi.org/10.22617/wps210305-2.

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Before the 1990s, Mongolia had a health care system that largely depended on hospital-based services. The country’s hospital sector was characterized by the extensive use of an excessive number of acute beds, a large number of medically unjustified admissions, and lengthy hospital stays. In the early 1990s, the Government of Mongolia started socioeconomic reforms as part of the transition to a market economy. It requested the Asian Development Bank (ADB) to support health sector reforms in the country. This paper describes the hospital sector in Mongolia along with the reforms and results achieved, challenges that remain, and ongoing and future directions for ADB support to better respond to the needs of the people.
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Alessa, Mohammed, Tayba Wahedi, Jumanah Alsairafi, Nouf Almatrafi, Wisal Shuaib, Johara Alnafie, Fatimah Alzubaidi, and Soha Elmorsy. Prevalence of Thyroid cancer in Saudi Arabis: Systematic review and Meta-analysis. INPLASY - International Platform of Registered Systematic Review and Meta-analysis Protocols, September 2022. http://dx.doi.org/10.37766/inplasy2022.9.0088.

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Review question / Objective: What is the prevalence of Thyroid cancer among population in kingdom of Saudi Arabia?. The aim of this systematic review is to scrutinize the prevalence of thyroid cancer (TC) in Saudi Arabia and assess the relative frequency of subgroups related to types of thyroid cancer, age, and gender. Condition being studied: Thyroid cancer is an abnormal growth of cells that starts in the thyroid gland. There is four types of differentiated thyroid cancer, three of these cancer develop from the follicular cells, the papillary thyroid cancer, follicular thyroid cancer, Hürthle cell carcinoma, and one rare type develops from the thyroid’s C cells called medullary thyroid cancer. There is one undifferentiated thyroid cancer called anaplastic thyroid cancer.
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Zilberman, Mark. Shouldn’t Doppler 'De-boosting' be accounted for in calculations of intrinsic luminosity of Standard Candles? Intellectual Archive, September 2021. http://dx.doi.org/10.32370/iaj.2569.

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"Doppler boosting / de-boosting" is a well-known relativistic effect that alters the apparent luminosity of approaching/receding radiation sources. "Doppler boosting" alters the apparent luminosity of approaching light sources to appear brighter, while "Doppler de-boosting" alters the apparent luminosity of receding light sources to appear fainter. While "Doppler boosting / de-boosting" has been successfully accounted for and observed in relativistic jets of AGN, double white dwarfs, in search of exoplanets and stars in binary systems it was ignored in the establishment of Standard Candles for cosmological distances. A Standard Candle adjustment appears necessary for "Doppler de-boosting" for high Z, otherwise we would incorrectly assume that Standard Candles appear dimmer, not because of "Doppler de-boosting" but because of the excessive distance, which would affect the entire Standard Candles ladder at cosmological distances. The ratio between apparent (L) and intrinsic (Lo) luminosities as a function of redshift Z and spectral index α is given by the formula ℳ(Z) = L/Lo=(Z+1)^(α-3) and for Type Ia supernova as ℳ(Z) = L/Lo=(Z+1)^(-2). These formulas are obtained within the framework of Special Relativity and may require adjustments within the General Relativity framework.
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Throckmorton, Hodges T., and Allan Lundy. Analysis of, Continuation of, and Report on Data Gathered at Dover AFB Mortuary during Operation Desert Storm: ARO Short Term Analysis Service Program (STAS). Subtitle: Anticipated and Actual Stress of Deployment to the Dover AFB Mortuary during Operation Desert Storm. Fort Belvoir, VA: Defense Technical Information Center, October 1992. http://dx.doi.org/10.21236/ada258991.

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Tiruneh, Dawit T., John Hoddinott, Caine Rolleston, Ricardo Sabates, and Tassew Woldehanna. Understanding Achievement in Numeracy Among Primary School Children in Ethiopia: Evidence from RISE Ethiopia Study. Research on Improving Systems of Education (RISE), May 2021. http://dx.doi.org/10.35489/bsg-rise-wp_2021/071.

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Ethiopia has succeeded in rapidly expanding access to primary education over the past two decades. However, learning outcomes remain low among primary school children and particularly among girls and children from disadvantaged backgrounds. Starting with a systematic review of quantitative studies on the determinants of learning outcomes among primary school children in Ethiopia, this study then examined key determinants of students’ numeracy achievement over the 2018-19 school year. The study focused on Grade 4 children (N=3,353) who are part of an on-going longitudinal study. The two questions that guided this study are: what are the key determinants of numeracy achievement at Grade 4 in primary schools in Ethiopia, and how does our current empirical study contribute to understanding achievement differences in numeracy among primary school children in Ethiopia? We employed descriptive and inferential statistics to examine factors that determine differences in numeracy scores at the start and end of the school year, as well as determinants of numeracy scores at the end of the school year conditional on achievement at the start of the school year. We examined differences across gender, region, and rural-urban localities. We also used ordinary least squares and school ‘fixed effects’ approaches to estimate the key child, household and school characteristics that determine numeracy scores in Grade 4. The findings revealed that boys significantly outperformed girls in numeracy both at the start and end of the 2018/19 school year, but the progress in numeracy scores over the school year by boys was similar to that of girls. Besides, students in urban localities made a slightly higher progress in numeracy over the school year compared to their rural counterparts. Students from some regions (e.g., Oromia) demonstrated higher progress in numeracy over the school year relative to students in other regions (e.g., Addis Ababa). Key child (e.g., age, health, hours spent per day studying at home) and school- and teacher-related characteristics (e.g., provision of one textbook per subject for each student, urban-rural school location, and teachers’ mathematics content knowledge) were found to be significantly associated with student progress in numeracy test scores over the school year. These findings are discussed based on the reviewed evidence from the quantitative studies in Ethiopia.
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Hajdini, Ina, Edward S. Knotek, John Leer, Mathieu O. Pedemonte, Robert W. Rich, and Raphael S. Schoenle. Indirect Consumer Inflation Expectations: Theory and Evidence. Federal Reserve Bank of Cleveland, November 2022. http://dx.doi.org/10.26509/frbc-wp-202235.

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Based on indirect utility theory, we introduce a novel methodology of measuring inflation expectations indirectly. This methodology starts at the individual level, asking consumers about the change in income required to buy the same amounts of goods and services one year ahead. Analytically, our methodology possesses smaller ex-post aggregate inflation forecast errors relative to forecasts based on conventional survey questions. We ask this question in a large-scale, high-frequency survey of consumers in the US and 14 countries, and we show that indirect consumer inflation expectations perform well along several empirical dimensions. Exploiting the geographically detailed, high-frequency variation in the data, we then show that individual experiences matter for inflation expectations, in a nuanced way. For example, age and gender have different effects internationally, while individual inflation and local experiences are generally highly relevant. In an application to gasoline price changes, we identify large effects of experienced gasoline price changes on inflation expectations, characterized by both overreaction and persistence.
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Melidis, Konstantin, and Markus Gruber. Begleitende Evaluierung IWB/EFRE AT 2014-20. Leistungspaket 1: Prioritätsachse 1 – Forschung, technologische Entwicklung und Innovation. Endbericht. Convelop gmbh, February 2022. http://dx.doi.org/10.22163/fteval.2022.582.

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Die Geschäftsstelle der Österreichischen Raumordnungskonferenz (ÖROK GSt.) hat als Verwaltungsbehörde des österreichischen IWB/EFRE -Programms die Durchführung einer begleitenden Evaluierung des Programms beauftragt, die mit Zuschlagserteilung der Bundesbeschaffung GmbH vom 07.12.2017 an ein Konsortium bestehend aus ÖIR, convelop, KMUFA, ÖAR, ÖGUT sowie Spatial Foresight ging. Die Evaluierung wird in mehreren Leistungspaketen bearbeitet, die sich im Wesentlichen auf die Prioritätsachsen des Programms beziehen, ergänzt um Evaluierungen zu den Bereichen „Governance“, „Kommunikation“ und „Querschnittsthemen“. Die gegenständliche Evaluierung ist ein Bestandteil dieser begleitenden Evaluierung und befasst sich im Kern mit den Maßnahmen der Priorität 1 „Stärkung der regionalen Wettbewerbsfähigkeit durch Forschung, technologische Entwicklung und Innovation“, ergänzt um die Maßnahme 15 „F&I in CO2-Reduktionstechnologien“ (P3) sowie die Maßnahmen 16 „F&T-Infrastruktur (Wien)“ und 17 „Innovationsdienstleistungen (Wien)“ (beide PA4). Mit 226,4 Mio. € decken die behandelten Maßnahmen 42% der EFRE-Mittel des Gesamtprogramms ab. Die Evaluierung zeichnet insgesamt ein überwiegend positives Bild der FTI-Förderung im EFRE, das es gilt, auch in Zukunft aufrechtzuerhalten. Die Empfehlungen der FTI-Evaluierung zielen vor allem auf eine noch klarere Konzeption und Darstellung von FTI-Maßnahmen mit grundsätzlich unterschiedlichen Wirkungslogiken und eine Weiterführung bestehender Bemühungen zur Harmonisierung regional unterschiedlicher Abwicklungsmodi innerhalb dieser Maßnahmen ab. Daneben sollte der Anspruch der Anwendungsorientierung im Lichte der stark wahrgenommenen Grundlagenorientierung in der Praxis reflektiert werden. Auch im Bereich der Datenerfassung und -qualitätsicherung wurden Ansatzpunkte für Verbesserungen aufgezeigt.
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Kislev, Yoav, Ramon Lopez, and Ayal Kimhi. Intergenerational Transfers by Farmers under Different Institutional Environments. United States Department of Agriculture, April 1995. http://dx.doi.org/10.32747/1995.7604936.bard.

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This research studies the issues of intergenerational transfers in general and farm succession in particular in two different institutional environments. One is the relatively unregulated farm sector in the United States, and the other is the heavily regulated family farms in Israeli moshavim. Most of the analysis is based on modern economic theory dealing with inheritance and other intergenerational issues. However, we start with two background studies. One is a review of the legal system affecting farm succession in the moshav, which, as we claim throughout the report, is of major importance to the question in hand. The second is an ethnographical study aimed at documenting various inheritance and succession practices in different moshavim. These two studies provide insight for most of the economic studies included here. The theoretical studies mostly deal with various aspects of two major decisions faced by farmers: who will succeed them on the farm, and when will succession take place. The first decision clearly depends on the institutional structure: for instance, Israeli farmers are limited to one successor while American farmers are not. The second decision can be taken in three stages: sharing farm work with the successor, sharing farm management, and eventually transferring the ownership. The occurrence and length of each stage depend on the first decision as well as on the institutional structure directly. The empirical studies are aimed at analyzing the practices and considerations of Israeli and American farmers regarding various intergenerational transfers-related issues. We found that American farmers' decisions are mainly driven by the desire to let the farm prosper in future generations and by a preference for equal treatment of heirs, and not at all by old-age support considerations. In contrast, we demonstrate the significant effect of old-age support on the value of the transferred farm in a sample of Israeli farms. Using Israeli census data, we find that the time of farm ownership transfer responds to economic incentives. A smaller Israeli panel data set shows that controlling for the occurrence of succession, farm size rises with operator's age and eventually falls, while intensity of production seems to decline steadily. This explains another finding, that farm transfer contributed significantly to farm growth when farming was attractive to successors. This finding supports our main conclusion, that the succession decisions are of major importance to the viability and profitability of family farms over the long run.
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Quak, Evert-jan. The Link Between Demography and Labour Markets in sub-Saharan Africa. Institute of Development Studies (IDS), January 2020. http://dx.doi.org/10.19088/k4d.2021.011.

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This rapid review synthesises the literature from academic, policy, and knowledge institution sources on how demography affects labour markets (e.g. entrants, including youth and women) and labour market outcomes (e.g. capital-per-worker, life-cycle labour supply, human capital investments) in the context of sub-Saharan Africa. One of the key findings is that the fast-growing population in sub-Saharan Africa is likely to affect the ability to get productive jobs and in turn economic growth. This normally happens when workers move from traditional (low productivity agriculture and household businesses) sectors into higher productivity sectors in manufacturing and services. In theory the literature shows that lower dependency ratios (share of the non-working age population) should increase output per capita if labour force participation rates among the working age population remain unchanged. If output per worker stays constant, then a decline in dependency ratio would lead to a rise in income per capita. Macro simulation models for sub-Saharan Africa estimate that capital per worker will remain low due to consistently low savings for at least the next decades, even in the low fertility scenario. Sub-Saharan African countries seem too poor for a quick rise in savings. As such, it is unlikely that a lower dependency ratio will initiate a dramatic increase in labour productivity. The literature notes the gender implications on labour markets. Most women combine unpaid care for children with informal and low productive work in agriculture or family enterprises. Large family sizes reduce their productive labour years significantly, estimated at a reduction of 1.9 years of productive participation per woman for each child, that complicates their move into more productive work (if available). If the transition from high fertility to low fertility is permanent and can be established in a relatively short-term period, there are long-run effects on female labour participation, and the gains in income per capita will be permanent. As such from the literature it is clear that the effect of higher female wages on female labour participation works to a large extent through reductions in fertility.
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