Thematische Bibliographien / Giant and subgiant stars

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Auswahl der wissenschaftlichen Literatur zum Thema „Giant and subgiant stars“

Autor: Grafiati
Veröffentlicht am 17. September 2021
Zuletzt aktualisiert am 11. Februar 2022

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Zeitschriftenartikel zum Thema "Giant and subgiant stars"

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Eggenberger, P., S. Deheuvels, A. Miglio, S. Ekström, C. Georgy, G. Meynet, N. Lagarde et al. „Asteroseismology of evolved stars to constrain the internal transport of angular momentum“. Astronomy & Astrophysics 621 (Januar 2019): A66. http://dx.doi.org/10.1051/0004-6361/201833447.

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Context. The observations of solar-like oscillations in evolved stars have brought important constraints on their internal rotation rates. To correctly reproduce these data, an efficient transport mechanism is needed in addition to the transport of angular momentum by meridional circulation and shear instability. The efficiency of this undetermined process is found to increase both with the mass and the evolutionary stage during the red giant phase. Aims. We study the efficiency of the transport of angular momentum during the subgiant phase. Methods. The efficiency of the unknown transport mechanism is determined during the subgiant phase by comparing rotating models computed with an additional corresponding viscosity to the asteroseismic measurements of both core and surface-rotation rates for six subgiants observed by the Kepler spacecraft. We then investigate the change in the efficiency of this transport of angular momentum with stellar mass and evolution during the subgiant phase. Results. The precise asteroseismic measurements of both core and surface-rotation rates available for the six Kepler targets enable a precise determination of the efficiency of the transport of angular momentum needed for each of these subgiants. These results are found to be insensitive to all the uncertainties related to the modelling of rotational effects before the post-main sequence (poMS) phase. An interesting exception in this context is the case of young subgiants (typical values of log(g) close to 4), because their rotational properties are sensitive to the degree of radial differential rotation on the main sequence (MS). These young subgiants constitute therefore perfect targets to constrain the transport of angular momentum on the MS from asteroseismic observations of evolved stars. As for red giants, we find that the efficiency of the additional transport process increases with the mass of the star during the subgiant phase. However, the efficiency of this undetermined mechanism decreases with evolution during the subgiant phase, contrary to what is found for red giants. Consequently, a transport process with an efficiency that increases with the degree of radial differential rotation cannot account for the core-rotation rates of subgiants, while it correctly reproduces the rotation rates of red giant stars. This suggests that the physical nature of the additional mechanism needed for the internal transport of angular momentum may be different in subgiant and red giant stars.
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Eggenberger, P., J. W. den Hartogh, G. Buldgen, G. Meynet, S. J. A. J. Salmon und S. Deheuvels. „Asteroseismology of evolved stars to constrain the internal transport of angular momentum“. Astronomy & Astrophysics 631 (November 2019): L6. http://dx.doi.org/10.1051/0004-6361/201936348.

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Context. Asteroseismic observations enable the characterisation of the internal rotation of evolved stars. These measurements reveal that an unknown efficient angular momentum (AM) transport mechanism is needed for subgiant and red giant stars in addition to hydrodynamic transport processes. A revised prescription for AM transport by the magnetic Tayler instability has been recently proposed as a possible candidate for such a missing mechanism. Aims. We compare the rotational properties predicted by this magnetic AM transport to asteroseismic constraints obtained for evolved stars with a particular focus on the subgiant phase. Methods. We computed models accounting for the recent prescription for AM transport by the Tayler instability with the Geneva stellar evolution code for subgiant and red giant stars, for which an asteroseismic determination of both core and surface rotation rates is available. Results. The revised prescription for the transport by the Tayler instability leads to low core rotation rates after the main sequence that are in better global agreement with asteroseismic measurements than those predicted by models with purely hydrodynamic processes or with the original Tayler-Spruit dynamo. A detailed comparison with asteroseismic data shows that the rotational properties of at most two of the six subgiants can be correctly reproduced by models accounting for this revised magnetic transport process. This result is obtained independently of the value adopted for the calibration parameter in this prescription. We also find that this transport by the Tayler instability faces difficulties in simultaneously reproducing asteroseismic measurements available for subgiant and red giant stars. The low values of the calibration parameter needed to correctly reproduce the rotational properties of two of the six subgiants lead to core rotation rates during the red giant phase that are too high. Inversely, the higher values of this parameter needed to reproduce the core rotation rates of red giants lead to a very low degree of radial differential rotation before the red giant phase, which is in contradiction with the internal rotation of subgiant stars. Conclusions. In its present form, the revised prescription for the transport by the Tayler instability does not provide a complete solution to the missing AM transport revealed by asteroseismology of evolved stars.
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Vauclair, S. „Turbulence and the Lithium Abundance in Giants and Main-Sequence Disk and Halo Stars“. Symposium - International Astronomical Union 145 (1991): 327–40. http://dx.doi.org/10.1017/s0074180900227472.

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The present situation concerning the observations of lithium in subgiant and giant stars is reviewed. These observations, compared to the determinations of lithium in main-sequence stars, can be used to obtain more stringents constraints on the dynamics of the stellar gas in the main-sequence as well as in the subgiant and giant stages. The macroscopic motions expected in stars are discussed from a theoretical point of view and compared to the observations, with special focusing on the theories of rotation-induced turbulence.
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Ruiz–Lapuente, Pilar, Jonay González Hernández, Hugo Tabernero, David Montes, Ramon Canal, Javier Mendez und Luigi Bedin. „Survey for the Binary Progenitor in SN1006 and Update on SN1572“. Proceedings of the International Astronomical Union 7, S281 (Juli 2011): 322–25. http://dx.doi.org/10.1017/s1743921312015293.

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AbstractWe have completed a survey down to R = 15 mag of the stars within a circle of 4 arcmin radius around the nominal center of the remnant of SN 1006, one of the three historical Type Ia supernovae (the other two being SN 1572 and SN 1604), in search of a possible surviving binary companion of the white dwarf whose explosion gave rise to the supernova. The stellar parameters (effective temperature, surface gravity, and metallicity), as well as the radial velocities of all the stars, have been measured from spectra obtained with the UVES spectrograph at the VLT, and from the former and the available photometry, distances have been determined. Chemical abundances of the Fe-peak elements Cr, Mn, Co, and Ni have also been measured to check for possible contamination of the stellar surface by the supernova ejecta. The limiting magnitude of the survey would allow us to find stellar companions of the red-giant type, subgiant stars, and main–sequence stars down to F5–6. Unlike in SN 1572, where a subgiant of type G0–1 has been proposed as the companion of SN 1572, for SN 1006 we can discard the possibility that SN 1006 had a red giant or subgiant companion.
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Pinçon, C., K. Belkacem, M. J. Goupil und J. P. Marques. „Can plume-induced internal gravity waves regulate the core rotation of subgiant stars?“ Astronomy & Astrophysics 605 (September 2017): A31. http://dx.doi.org/10.1051/0004-6361/201730998.

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Context. The seismic data provided by the space-borne missions CoRoT and Kepler enabled us to probe the internal rotation of thousands of evolved low-mass stars. Subsequently, several studies showed that current stellar evolution codes are unable to reproduce the low core rotation rates observed in these stars. These results indicate that an additional angular momentum transport process is necessary to counteract the spin up due to the core contraction during the post-main sequence evolution. For several candidates, the transport induced by internal gravity waves (IGW) could play a non-negligible role. Aims. We aim to investigate the effect of IGW generated by penetrative convection on the internal rotation of low-mass stars from the subgiant branch to the beginning of the red giant branch. Methods. A semi-analytical excitation model was used to estimate the angular momentum wave flux. The characteristic timescale associated with the angular momentum transport by IGW was computed and compared to the contraction timescale throughout the radiative region of stellar models at different evolutionary stages. Results. We show that IGW can efficiently counteract the contraction-driven spin up of the core of subgiant stars if the amplitude of the radial-differential rotation (between the center of the star and the top of the radiative zone) is higher than a threshold value. This threshold depends on the evolutionary stage and is comparable to the differential rotation rates inferred for a sample of subgiant stars observed by the satellite Kepler. Such an agreement can therefore be interpreted as the consequence of a regulation mechanism driven by IGW. This result is obtained under the assumption of a smooth rotation profile in the radiative region and holds true even if a wide range of values is considered for the parameters of the generation model. In contrast, on the red giant branch, we find that IGW remain insufficient, on their own, to explain the observations because of an excessive radiative damping. Conclusions. IGW generated by penetrative convection are able to efficiently extract angular momentum from the core of stars on the subgiant branch and accordingly have to be taken into account. Moreover, agreements with the observations reinforce the idea that their effect is essential to regulate the amplitude of the radial-differential rotation in subgiant stars. On the red giant branch, another transport mechanism must likely be invoked.
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Hekker, S., und A. Mazumdar. „Solar-like oscillations in subgiant and red-giant stars: mixed modes“. Proceedings of the International Astronomical Union 9, S301 (August 2013): 325–31. http://dx.doi.org/10.1017/s1743921313014531.

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AbstractThanks to significant improvements in high-resolution spectrographs and the launch of dedicated space missions MOST, CoRoT and Kepler, the number of subgiants and red-giant stars with detected oscillations has increased significantly over the last decade. The amount of detail that can now be resolved in the oscillation patterns does allow for in-depth investigations of the internal structures of these stars. One phenomenon that plays an important role in such studies are mixed modes. These are modes that carry information of the inner radiative region as well as from the convective outer part of the star allowing to probe different depths of the stars.Here, we describe mixed modes and highlight some recent results obtained using mixed modes observed in subgiants and red-giant stars.
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Pinçon, C., K. Belkacem und M. J. Goupil. „Excitation of internal gravity waves by penetrative convection“. EAS Publications Series 82 (2019): 247–51. http://dx.doi.org/10.1051/eas/1982024.

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We investigate the ability of internal gravity waves that are generated by penetrative convection to redistribute angular momentum in the internal radiative zone of evolved low-mass stars. To do so, we use the semianalytical excitation model recently proposed by Pinçon et al. 2016. We briefly report the preliminary results of the study focusing on the subgiant and red giant branch stars.
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Hon, Marc, Dennis Stello, Rafael A. García, Savita Mathur, Sanjib Sharma, Isabel L. Colman und Lisa Bugnet. „A search for red giant solar-like oscillations in all Kepler data“. Monthly Notices of the Royal Astronomical Society 485, Nr. 4 (04.03.2019): 5616–30. http://dx.doi.org/10.1093/mnras/stz622.

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ABSTRACT The recently published Kepler mission Data Release 25 (DR25) reported on ∼197 000 targets observed during the mission. Despite this, no wide search for red giants showing solar-like oscillations have been made across all stars observed in Kepler’s long-cadence mode. In this work, we perform this task using custom apertures on the Kepler pixel files and detect oscillations in 21 914 stars, representing the largest sample of solar-like oscillating stars to date. We measure their frequency at maximum power, νmax, down to $\nu _{\mathrm{max}}\simeq 4\, \mu$Hz and obtain log (g) estimates with a typical uncertainty below 0.05 dex, which is superior to typical measurements from spectroscopy. Additionally, the νmax distribution of our detections show good agreement with results from a simulated model of the Milky Way, with a ratio of observed to predicted stars of 0.992 for stars with $10 \lt \nu _{\mathrm{max}}\lt 270\, \mu$Hz. Among our red giant detections, we find 909 to be dwarf/subgiant stars whose flux signal is polluted by a neighbouring giant as a result of using larger photometric apertures than those used by the NASA Kepler science processing pipeline. We further find that only 293 of the polluting giants are known Kepler targets. The remainder comprises over 600 newly identified oscillating red giants, with many expected to belong to the Galactic halo, serendipitously falling within the Kepler pixel files of targeted stars.
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Simon, Theodore, und Stephen A. Drake. „The evolution of chromospheric activity of cool giant and subgiant stars“. Astrophysical Journal 346 (November 1989): 303. http://dx.doi.org/10.1086/168012.

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Corsaro, E., J. M. McKeever und J. S. Kuszlewicz. „Fast and Automated Peak Bagging with DIAMONDS (FAMED)“. Astronomy & Astrophysics 640 (August 2020): A130. http://dx.doi.org/10.1051/0004-6361/202037930.

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Stars of low and intermediate mass that exhibit oscillations may show tens of detectable oscillation modes each. Oscillation modes are a powerful tool to constrain the internal structure and rotational dynamics of the star, hence allowing one to obtain an accurate stellar age. The tens of thousands of solar-like oscillators that have been discovered thus far are representative of the large diversity of fundamental stellar properties and evolutionary stages available. Because of the wide range of oscillation features that can be recognized in such stars, it is particularly challenging to properly characterize the oscillation modes in detail, especially in light of large stellar samples. Overcoming this issue requires an automated approach, which has to be fast, reliable, and flexible at the same time. In addition, this approach should not only be capable of extracting the oscillation mode properties of frequency, linewidth, and amplitude from stars in different evolutionary stages, but also able to assign a correct mode identification for each of the modes extracted. Here we present the new freely available pipeline FAMED (Fast and AutoMated pEak bagging with DIAMONDS), which is capable of performing an automated and detailed asteroseismic analysis in stars ranging from the main sequence up to the core-helium-burning phase of stellar evolution. This, therefore, includes subgiant stars, stars evolving along the red giant branch (RGB), and stars likely evolving toward the early asymptotic giant branch. In this paper, we additionally show how FAMED can detect rotation from dipolar oscillation modes in main sequence, subgiant, low-luminosity RGB, and core-helium-burning stars.
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Dissertationen zum Thema "Giant and subgiant stars"

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Thorén, Patrik. „Dwarf and Subgiant Stars as Probes of Galactic Chemical and Dynamical Evolution“. Doctoral thesis, Uppsala universitet, Uppsala Astronomiska Observatorium, 2001. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-636.

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Stellar chemical abundances provide astronomers with vital information about the production of chemical elements. Some stars preserve the composition of the environment in which they were born on their surfaces. By analysing the light from a star, the abundances of elements, its age and its path in space can be derived, and translated into the language of galactic history. The spallative history of boron in the early Galaxy was reinvestigated by observations of an ultraviolet spectral line in the old star HD 140283 with the Hubble Space Telescope. The line was barely detected and the upper limit abundance derived was lower than expected, which calls for further observations of this line in halo stars. Stars evolved into subgiants were observed with the ESO CAT, La Silla, and NOT, La Palma, to deduce their usefulness for galactic evolution studies. The high resolution spectroscopy study of the 26 objects showed that these stars are indeed useful for such studies. They are more luminous than dwarf stars and their ages can be accurately derived. They do not seem to have changed their surface abundances due to their evolution into giants. Subgiants can successfully be used to observationally reach regions further from the Earth, which can remove local biases that may appear when only observing nearby dwarf stars. A NLTE investigation of neutral Ca showed that cool metal rich dwarf stars did not deviate significantly from LTE, as had earlier been suggested. By an LTE analysis of a sample of 17 such dwarfs, using recent MARCS atmospheres, synthetic spectroscopy and modern atomic line data, cool metal rich dwarfs were shown not to deviate significantly from the expected abundance patterns in a number of elements. This increases the number of potential targets for studies of galactic chemical evolution in the metal rich regime since most stars are cool.
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Thorén, Patrik. „Dwarf and subgiant stars as probes of galactic chemical and dynamical evolution /“. Uppsala : Acta Universitatis Upsaliensis : Univ.-bibl. [distributör], 2001. http://publications.uu.se/theses/91-554-4991-3/.

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Ortiz, Mauricio, Sabine Reffert, Trifon Trifonov, Andreas Quirrenbach, David S. Mitchell, Grzegorz Nowak, Esther Buenzli et al. „Precise radial velocities of giant stars“. EDP SCIENCES S A, 2016. http://hdl.handle.net/10150/622444.

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Context. For over 12 yr, we have carried out a precise radial velocity (RV) survey of a sample of 373 G- and K-giant stars using the Hamilton Echelle Spectrograph at the Lick Observatory. There are, among others, a number of multiple planetary systems in our sample as well as several planetary candidates in stellar binaries. Aims. We aim at detecting and characterizing substellar and stellar companions to the giant star HD 59686 A (HR 2877, HIP 36616). Methods. We obtained high-precision RV measurements of the star HD 59686 A. By fitting a Keplerian model to the periodic changes in the RVs, we can assess the nature of companions in the system. To distinguish between RV variations that are due to non-radial pulsation or stellar spots, we used infrared RVs taken with the CRIRES spectrograph at the Very Large Telescope. Additionally, to characterize the system in more detail, we obtained high-resolution images with LMIRCam at the Large Binocular Telescope. Results. We report the probable discovery of a giant planet with a mass of m(p) sin i = 6.92(-0.24)(+0.18) M-Jup orbiting at a(p) = 1.0860(-0.0007)(+0.0006) aufrom the giant star HD 59686 A. In addition to the planetary signal, we discovered an eccentric (e(B) = 0.729(-0.003)(+0.004)) binary companionwith a mass of m(B) sin i = 0.5296(-0.0008)(+0.0011) M-circle dot orbiting at a close separation from the giant primary with a semi-major axis of a(B) = 13.56(-0.14)(+0.18) au. Conclusions. The existence of the planet HD 59686 Ab in a tight eccentric binary system severely challenges standard giant planet formation theories and requires substantial improvements to such theories in tight binaries. Otherwise, alternative planet formation scenarios such as second-generation planets or dynamical interactions in an early phase of the system's lifetime need to be seriously considered to better understand the origin of this enigmatic planet.
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Papakonstantinou, Nikolaos. „Examining LUMBA UVES pipeline spectroscopy on giant and sub-giant stars of M67“. Thesis, Uppsala universitet, Observationell astrofysik, 2021. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-448637.

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In this work, the efficiency of the LUMBA UVES pipeline for processing of spectroscopic observations is tested by use on 23 high-resolution spectra of the open star cluster M67. An abundance trend discovered by Gavel et al. (2019) concerning iron abundances of giant and sub-giant stars of that cluster is examined. An initial run for a set of ”Gaia FGK benchmark stars”, as described in Blanco-Cuaresma et al. (2014) and Heiter et al. (2015) helps inspect the structure, method and output of the pipeline. Through Python language programming, processes are greatly automatized and the pipeline is run for a total of 460 weak and strong iron lines of our 23-star sample. The line fitting and efficiency of the pipeline is appreciated by statistically analyzing the results and looking into individual discrepant ones. The abundance trend is reproduced while using FeI lines, unlike runs using FeII lines. Trends in abundance over line strength plots also hint at bias through the Gaia-Eso Survey (GES) microturbulence relation. Using internal Data Release 6 (iDR6) and LUMBA-derived starting parameters, log(g) - Teff plots of our sample stars agree with a previously established 4.3 Gyr cluster age. An alternate run is performed for those stars, using LUMBA-derived starting parameters. The choice of starting parameters does impact abundance derivation, but is not the primary source of persistent systematic discrepancies.
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Willems, Frits Jan. „Infrared studies of asymptotic giant branch stars“. [S.l. : Amsterdam : s.n.] ; Universiteit van Amsterdam [Host], 1987. http://dare.uva.nl/document/113520.

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Norgren, Ofelia. „Pulsation Properties in Asymptotic Giant Branch Stars“. Thesis, Uppsala universitet, Teoretisk astrofysik, 2019. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-388388.

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Asymptotic Giant Branch (AGB) stars are stars with low- to intermediate mass in a late stage in their stellar evolution. An important feature of stellar evolution is the ongoing nucleosynthesis, the creation of heavier elements. Unlike main sequence stars, the AGB stars have a thick convective envelope which makes it possible to dredge-up the heavier fused elements from the stellar core to its surface. AGB stars are also pulsating variable stars, meaning the interior expands and contracts, causing the brightness to fluctuate. These pulsations will also play a major role in the mass loss observed in these stars. The mass loss is caused by stellar winds that accelerate gas and dust from the surface of these stars and thereby chemical enrich the interstellar medium. It is important to understand the properties of these pulsations since they play a key role in how stellar winds are produced and then enrich the galaxy with heavier synthesized elements. These pulsation periods can be observed with their corresponding Light-Curves, where the periodic motion of the brightness can be clearly seen. The main goal with this project is to calculate these pulsation periods for different AGB stars and compare these values with the periods listed in the General Catalogue of Variable Stars (GCVS). The comparison between these values gives a better understanding of methods of determining these periods and the uncertainties that follow.
Asymptotiska jättegrenen är en del av slutstadiet för låg- till medelmassiva stjärnor (AGB stjärnor). Ett viktigt kännetecken hos stjärnutvecklingen är den pågående nukleosyntesen, sammanslagningen av tyngre ämnen i stjärnans inre. Till skillnad mot stjärnor på huvudserien har AGB stjärnor ett tjockt konvektivt lager som gör det möjligt att dra upp dessa nybildade ämnen till stjärnans yta. AGB stjärnor är pulserande variabla stjärnor där variationer i stjärnans radie gör att ljusstyrkan varierar. Dessa pulsationer kommer även att spela en viktig roll för den massförlust som observeras hos dessa stjärnor. Massförlusten orsakas av stjärnvindar som accelererar gas och stoft från stjärnans yta och därmed kemiskt berikar det interstellära mediet. Det är viktigt att förstå dessa pulsationer eftersom de är en viktig komponent för hur stjärnvindar uppstår och sedan berikar galaxer med tyngre ämnen. Dessa pulsationsperioder kan studeras genom att observera stjärnornas ljuskurvor, där man tydligt ser det periodiska beteendet hos ljusstyrkan. Det huvudsakliga målet med detta projekt är att beräkna dessa perioder för olika AGB stjärnor och att sedan jämföra dem med värden från General Catalogue of Variable Stars (GCVS). Jämförelsen mellan dessa värden ger en bättre förståelse för metoderna som används för att bestämma dessa perioder och hur osäkra dessa värden är.
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Van, Eck Sophie. „Binary intruders among peculiar red giant stars“. Doctoral thesis, Universite Libre de Bruxelles, 1999. http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/211875.

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COOK, KEM HOLLAND. „ASYMPTOTIC GIANT BRANCH POPULATIONS IN COMPOSITE STELLAR SYSTEMS“. Diss., The University of Arizona, 1987. http://hdl.handle.net/10150/184208.

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This dissertation presents a technique for the identification and classification of late-type stars and for the estimation of M star metallicities. The technique uses broad-band, V and I, CCD images to identify red stars and two intermediate-band CCD images to classify these as carbon or M types. One of the intermediate passbands is centered on a TiO absorption band at 7750Å and the other is centered on a CN absorption band at 8100Å. Color-color plots of V-I versus the intermediate-band index, 77-81, clearly distinguishes carbon from M stars. Observations of both early- and late-type stars were used to define the 77-81 system based upon the intermediate-band filters. The TiO bandstrength deduced from the 77-81 color as a function of V-I color was investigated for field giants and giants in 12 globular clusters. A linear correlation between [Fe/H] and the V-I color at a given TiO bandstrength was found. This correlation can be used to estimate the metallicity of M giants. The stellar population of a field in Baade's Window was examined using this technique. Many late-M stars and no carbon stars were found. The color-color diagram for Baade's Window suggests a range of metallicities for the M giants of [Fe/H] ≈ -0.4 to > +0.2. The stellar population of the Sagittarius Dwarf Irregular galaxy (Sagdig) was examined using the 77-81 system. A method for estimating reddening based upon the color mode of foreground stars was developed for the analysis of the Sagdig data. Sagdig is estimated to be ~ 1.3 megaparsecs distant. Bright blue and red stars in Sagdig are evidence for recent star formation. Carbon stars were identified in Sagdig. They display a bimodal luminosity and color distribution which suggests distinct epochs of star forming activity between 1 and 10 Gyr ago. The spatial distribution of carbon stars and bright red stars in Sagdig shows this galaxy to be much larger than previously thought.
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Weldrake, David Thomas Fredrick, und weldrake@mpia-hd mpg de. „Giant Planets and Variable Stars in Globular Clusters“. The Australian National University. Research School of Astronomy and Astrophysics, 2005. http://thesis.anu.edu.au./public/adt-ANU20050616.191315.

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Over the last decade, 135 extrasolar planets have been discovered, the vast majority found by ongoing radial velocity searches. Of the stars sampled in these searches, 1% have `Hot Jupiter' planets associated with them. Having masses equivalent to Jupiter yet orbital periods of only a few days, this new class of planet is clearly unlike anything in our Solar System.¶ Hot Jupiters present us with an intriguing prospect. If the orientation of the planetary orbit is close to edge-on, the planet will periodically transit across the face of its star, resulting in a small drop in brightness. This transit phenomenon has been successfully used for planet detection over the last couple of years, allowing determination of the planetary radius and accurate mass estimates when coupled with radial velocity observations.¶ To aid understanding of the effect stellar environment plays on Hot Jupiter formation and survivability, this thesis presents the results of a wide-field search for transiting Hot Jupiters in the globular cluster 47 Tucanae. This cluster presents many thousands of stars in a moderate field of view and provides the perfect target for a search of this nature. One previous transit search has been made in the central core of 47 Tuc; using the HST for 8.3 continuous days, Gilliland et.al (2000) expected 17 transits yet found none. This null result suggests that either system metallicity or stellar density may be inhibiting Hot Jupiter formation or survivability in the cluster.¶ This thesis presents a search for transits with a field of view 250 times larger than the HST search and samples the uncrowded outer halo of the cluster (previously unsampled for transits), providing important constraints on the effect of environment on Hot Jupiter formation. If planets are found, then stellar density would seem responsible for the Gilliland et.al (2000) core null result. If no planets are found to a significant level, the survey would provide strong evidence that system metallicity is the dominant factor. Using the ANU 40'' (1m) telescope at Siding Spring Observatory, a 30.4 night observing run was executed and photometry was derived via differential imaging. The dataset numbers 109,000 cluster (and field) stars for photometric analysis, of which 22,000 are suitable for the transit search. With a custom-written transit detection algorithm and extensive Monte Carlo simulations to model the dataset, seven planets should be detectable if the occurrence rate of Hot Jupiters is the same in the cluster as in the Solar Neighbourhood.¶ Despite a detailed search, no transit signatures were identified. This result strongly indicates that the low metallicity of the cluster is the dominant factor inhibiting planet formation in 47 Tuc. Current results in the Solar Neighbourhood show that planet frequency is strongly biased towards stars of high metallicity. This thesis shows that the metallicity trend is likely a universal phenomenon, not only limited to the immediate Solar Neighbourhood and raises questions of whether planets were much rarer in the earlier Universe.¶ As a side result of the search, 100 variable stars were identified in the field, 69 of which are new discoveries. Subsequent analysis reveals a strong period segregation among the cluster eclipsing binaries, indicating previously unobserved dynamical effects in the cluster. Distance estimates for both 47 Tuc and the SMC are in agreement with previously published values and an independent identification of the binary period-colour relation was observed. Two binaries seem to have low-luminosity companions worthy of followup and one variable is likely a star in the early phases of planetary nebula formation. All of the results presented in this thesis have been published in three separately refereed research papers.
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Weldrake, David Thomas Frederick. „Giant planets and variable stars in globular clusters /“. View thesis entry in Australian Digital Theses Program, 2005. http://thesis.anu.edu.au/public/adt-ANU20050616.191315/index.html.

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Bücher zum Thema "Giant and subgiant stars"

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Habing, Harm J., und Hans Olofsson, Hrsg. Asymptotic Giant Branch Stars. New York, NY: Springer New York, 2004. http://dx.doi.org/10.1007/978-1-4757-3876-6.

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Aguilera-Gómez, Claudia. Explaining Lithium Enriched Red Giant Branch Stars. Cham: Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-030-02583-0.

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The giant leap: Mankind heads for the stars. London: Headline, 1999.

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Berry, Adrian. The giant leap: Mankind heads for the stars. London: Headline, 1999.

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Berry, Adrian. The giant leap: Mankind heads for the stars. London: Headline, 2000.

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Harpaz, Amos. The rings around the egg nebula. [Washington, DC: National Aeronautics and Space Administration, 1998.

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Harpaz, Amos. The rings around the egg nebula. [Washington, DC: National Aeronautics and Space Administration, 1998.

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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. Herausgegeben von Astronomical Society of the Pacific. San Francisco: Astronomical Society of the Pacific, 2011.

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Chadney, Joshua. Modelling the Upper Atmosphere of Gas-Giant Exoplanets Irradiated by Low-Mass Stars. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-63351-0.

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T, Le Bertre, Lèbre A, Waelkens C und International Astronomical Union, Hrsg. Asymptotic giant branch stars: Proceedings of the 191st Symposium of the International Astronomical Union held in Montpellier, France, 27 August-1 September 1998. San Francisco, CA: Astronomical Society of the Pacific, 1999.

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Buchteile zum Thema "Giant and subgiant stars"

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Fischer, Daniel, und Hilmar Duerbeck. „Giant Stars“. In Hubble Revisited, 112–17. New York, NY: Springer New York, 1998. http://dx.doi.org/10.1007/978-1-4612-2232-3_16.

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Straniero, O., M. Limongi, A. Chieffi, R. Gallino und M. Busso. „Asymptotic Giant Branch Stars“. In The Evolution of The Milky Way, 429–43. Dordrecht: Springer Netherlands, 2000. http://dx.doi.org/10.1007/978-94-010-0938-6_42.

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Hatzes, A. P., M. Döllinger, L. Pasquini, J. Setiawan, L. Girardi und L. da Silva. „Planets Around Giant Stars“. In Precision Spectroscopy in Astrophysics, 197–200. Berlin, Heidelberg: Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-75485-5_42.

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Pinheiro, F. J. G., und J. M. Fernandes. „Asteroseismology and the degeneracy of model solutions for subgiant stars“. In Synergies between Solar and Stellar Modelling, 71–76. Dordrecht: Springer Netherlands, 2009. http://dx.doi.org/10.1007/978-90-481-9198-7_9.

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Mowlavi, Nami. „Nucleosynthesis in Red Giant Stars“. In Cosmic Chemical Evolution, 57–69. Dordrecht: Springer Netherlands, 2002. http://dx.doi.org/10.1007/978-94-010-0452-7_6.

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Griffiths, Martin. „Giant Stars and Their Variability“. In The Patrick Moore Practical Astronomy Series, 111–33. Cham: Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-030-00904-5_7.

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Stevenson, David J. „Gas and Ice Giant Interiors“. In Planets, Stars and Stellar Systems, 195–221. Dordrecht: Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5606-9_4.

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Knapp, G. R., C. F. Gammie, K. Young und T. G. Phillips. „CO Observations of Evolved Giant Stars“. In Submillimetre Astronomy, 33–34. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-015-6850-0_9.

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Martin, F., und S. J. McCarthy. „Harlow Shapley and Red Giant Stars“. In The Harlow-Shapley Symposium on Globular Cluster Systems in Galaxies, 481–82. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-015-1104-9_70.

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Bally, John, und David Devine. „Giant Herbig-Haro Flows“. In Herbig-Haro Flows and the Birth of Low Mass Stars, 29–38. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-011-5608-0_3.

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Konferenzberichte zum Thema "Giant and subgiant stars"

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MACIEL, S. C., D. B. DE FREITAS und J. R. DE MEDEIROS. „THE ROLE OF MAGNETIC BRAKING EFFECTS ON THE ROTATION OF SUBGIANT AND GIANT STARS“. In Proceedings of the Third Workshop (IWARA07). WORLD SCIENTIFIC, 2010. http://dx.doi.org/10.1142/9789814304887_0029.

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Cavallo, Robert M., Kem H. Cook, D. Minniti und T. Vandehei. „Preliminary abundance analysis of galactic bulge main sequence, subgiant, and giant branch stars observed during microlensing with Keck/HIRES“. In Astronomical Telescopes and Instrumentation, herausgegeben von Puragra Guhathakurta. SPIE, 2003. http://dx.doi.org/10.1117/12.457702.

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Quirrenbach, Andreas, Sabine Reffert und Christoph Bergmann. „Planets around Giant Stars“. In PLANETARY SYSTEMS BEYOND THE MAIN SEQUENCE: Proceedings of the International Conference. AIP, 2011. http://dx.doi.org/10.1063/1.3556189.

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El Eid, Mounib F. „Nucleosynthesis in asymptotic giant branch stars“. 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/10.1063/1.4875289.

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Pricopi, D., M. D. Suran, Joyce Ann Guzik und Paul A. Bradley. „Pulsational Stability of Red Giant Stars“. In STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION: Proceedings of the International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3246432.

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Smith, Verne V. „The chemical compositions of red giant stars“. In Cosmic abundances of matter. AIP, 1989. http://dx.doi.org/10.1063/1.38014.

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Whitelock, Patricia. „Large Telescopes and Asymptotic Giant Branch Stars“. In STELLAR ASTROPHYSICS WITH THE WORLD'S LARGEST TELESCOPES: First International Workshop on Stellar Astrophysics with the World's Largest Telescopes. AIP, 2005. http://dx.doi.org/10.1063/1.1893340.

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Jones, Matias I., James S. Jenkins und Patricio Rojo. „Study of Planetary Systems around Giant Stars“. In PLANETARY SYSTEMS BEYOND THE MAIN SEQUENCE: Proceedings of the International Conference. AIP, 2011. http://dx.doi.org/10.1063/1.3556217.

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Roche, Joseph, Brian R. Espey, Cian Crowley und Eric Stempels. „Exploring the Origin of Red Giant Winds“. In COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099260.

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Karakas, Amanda, Maria Lugaro und Roberto Gallino. „The Production of Germanium in Asymptotic Giant Branch stars“. In International Symposium on Nuclear Astrophysics - Nuclei in the Cosmos - IX. Trieste, Italy: Sissa Medialab, 2010. http://dx.doi.org/10.22323/1.028.0124.

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