Relevant bibliographies by topics / Lost in the stars

Contents

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

Academic literature on the topic 'Lost in the stars'

Author: Grafiati
Published: 4 June 2021
Last updated: 1 February 2022

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Journal articles on the topic "Lost in the stars"

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Cederna, Camilla Maria. "Lost stars." Sigila N�41, no. 1 (2018): 96. http://dx.doi.org/10.3917/sigila.041.0096.

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Lappin, Louis, Maxwell Anderson, and Kurt Weill. "Lost in the Stars." Theatre Journal 38, no. 4 (December 1986): 479. http://dx.doi.org/10.2307/3208293.

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Vink, Jorick S. "Mass loss and stellar superwinds." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 375, no. 2105 (September 18, 2017): 20160269. http://dx.doi.org/10.1098/rsta.2016.0269.

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Mass loss bridges the gap between massive stars and supernovae (SNe) in two major ways: (i) theoretically, it is the amount of mass lost that determines the mass of the star prior to explosion and (ii) observations of the circumstellar material around SNe may teach us the type of progenitor that made the SN. Here, I present the latest models and observations of mass loss from massive stars, both for canonical massive O stars, as well as very massive stars that show Wolf–Rayet type features. This article is part of the themed issue ‘Bridging the gap: from massive stars to supernovae’.
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Renzini, Alvio. "Hot Gas Flows in Elliptical Galaxies." Symposium - International Astronomical Union 171 (1996): 131–38. http://dx.doi.org/10.1017/s0074180900232257.

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Stars in elliptical galaxies lose mass at an overall present rate Ṁ∗ ≃ 1.5 × 10−11LBM⊙yr−1 (e.g., Faber & Gallagher 1976; Renzini & Buzzoni 1986). When allowing for the predicted increase back with cosmological time it turns out that over one Hubble time the stellar population of an elliptical galaxy has cumulatively lost 20-50% of its initial mass, the precise value depending on the IMF. This review focuses on two simple questions: what happens to the gas being lost by the stars? Where is it ultimately disposed?
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Gingerich, Owen. "Book Review: Troublesome Stars: Lost Stars: Lost, Missing, and Troublesome Stars from the Catalogues of Johannes Bayer, Nicholas-Louis de Lacaille, John Flamsteed, and Sundry others." Journal for the History of Astronomy 35, no. 2 (May 2004): 244–45. http://dx.doi.org/10.1177/002182860403500212.

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Liu, Cheng, Sofia Feltzing, and Gregory Ruchti. "Finding the lost siblings of the Sun." Proceedings of the International Astronomical Union 9, S298 (May 2013): 426. http://dx.doi.org/10.1017/s1743921313006923.

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AbstractWe have performed a spectral analysis on 18 stars solar sibling candidate. We found that only one one of the candidateshas solar metallicity and at the same time might have an age comparable to that of the Sun.
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Taylor, Philip, Chiaki Kobayashi, and Lisa J. Kewley. "Oxygen loss from simulated galaxies and the metal flow main sequence: predicting the dependence on mass and environment." Monthly Notices of the Royal Astronomical Society 496, no. 4 (July 7, 2020): 4433–41. http://dx.doi.org/10.1093/mnras/staa1904.

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ABSTRACT We predict the mass fraction of oxygen lost from galaxies in a cosmological simulation as a function of stellar mass and environment at the present day. The distribution with stellar mass is bimodal, separating star-forming and quenched galaxies. The metallicity of gas and stars is self-consistently calculated using a chemical evolution model that includes Type II and Ia supernovae, hypernovae, and asymptotic giant branch stars. The mass of oxygen lost from each galaxy is calculated by comparing the existing oxygen in gas and stars in the galaxy to the oxygen that should have been produced by the present-day population of stars. More massive galaxies are able to retain a greater fraction of their metals (∼100 per cent) than low-mass galaxies (∼40–70 per cent). As in the star formation main sequence, star-forming galaxies follow a tight relationship also in terms of oxygen mass lost – a metal flow main sequence – whereas massive quenched galaxies tend to have lost a greater fraction of oxygen (up to 20 per cent), due to active galactic nucleus-driven winds. The amount of oxygen lost by satellite galaxies depends on the details of their interaction history, and those in richer groups tend to have lost a greater fraction of their oxygen. Observational estimates of metal retention in galaxies will provide a strong constraint on models of galaxy evolution.
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Marston, Anthony P. "Ring nebulae: what they tell us about Wolf-Rayet stars." Symposium - International Astronomical Union 193 (1999): 306–15. http://dx.doi.org/10.1017/s0074180900205573.

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The environments of evolved massive stars provide an opportunity of obtaining information on the past, as well as current, condition of the stars themselves. In this review we will look at the incidence of ring nebulae around Wolf-Rayet stars, their differing morphologies at various wavelengths and the existence of multiple, concentric shells. We use this information to show that WRs are indeed evolved stars and that the various phases of evolution for a WR star are evidenced in their environments. Abundance measurements and kinematics show that complex forms of mass ejection are likely to have occurred in the evolution of WR stars providing clumpy structures of dust, and both ionized and neutral gas. Gas kinematics also provide estimates to the time-scales of each of the evolutionary phases of WR stars, which can be combined with estimates of nebular masses to provide the approximate values for such crucial parameters as total mass-loss and historical mass-loss rates. Overall, it is illustrated that studies of the environments of WR stars have the potential to provide important information about the mass-loss history of very massive stars, including estimates of the time period of each mass-loss phase, typical mass loss rates, total mass lost and likely evolutionary path. Some of the remaining problems relating to the use of ring nebulae as probes to the evolutionary history of WR stars are also discussed.
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Koch, Andreas, Eva K. Grebel, and Sarah L. Martell. "Purveyors of fine halos: Re-assessing globular cluster contributions to the Milky Way halo buildup with SDSS-IV." Astronomy & Astrophysics 625 (May 2019): A75. http://dx.doi.org/10.1051/0004-6361/201834825.

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There is ample evidence in the Milky Way for globular cluster (GC) disruption. It may therefore be expected that part of the Galactic halo field star population may also once have formed in GCs. We seek to quantify the fraction of halo stars donated by GCs by searching for stars that bear the unique chemical fingerprints typical for a subset of GC stars often dubbed “second-generation stars”. These are stars showing light-element abundance anomalies such as a pronounced CN-band strength accompanied by weak CH-bands. Based on this indicator, past studies have placed the fraction of halo stars with a GC origin between a few to up to 50%. Using low-resolution spectra from the most recent data release (DR14) of the latest extension of the Sloan Digital Sky Survey (SDSS-IV), we were able to identify 118 metal-poor (−1.8 ≤ [Fe/H] ≤ −1.3) CN-strong stars in a sample of 4470 halo giant stars out to ∼50 kpc. This increases the number of known halo stars with GC-like light-element abundances by a factor of two and results in an observed fraction of these stars of 2.6 ± 0.2%. Using an updated formalism to account for the fraction of stars lost early on in the GC evolution, we thus estimate the fraction of the Galactic halo that stems from disrupted clusters to be very low, at 11 ± 1%. This number would represent the case that stars lost from GCs were entirely from the first generation and is thus merely an upper limit. Our conclusions are sensitive to our assumptions of the mass lost early on from the first generation formed in the GCs, the ratio of first-to-second generation stars, and other GC parameters. We carefully tested the influence of varying these parameters on the final result and find that under realistic scenarios, this fraction depends on the main assumptions at less than 10 percentage points. We further recover a flat trend in this fraction with Galactocentric radius, with a marginal indication of a rise beyond 30 kpc that could reflect the ex situ origin of the outer halo as is also seen in other stellar tracers.
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Glanz, J. "Astronomy: Dust Grains Bring Long-Lost Stars Into the Laboratory." Science 274, no. 5290 (November 15, 1996): 1078a—1079. http://dx.doi.org/10.1126/science.274.5290.1078a.

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Dissertations / Theses on the topic "Lost in the stars"

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Young, Kenneth Harbour Phillips Thomas G. "Submillimeter and infrared studies of mass lost by asymptotic giant branch stars /." Diss., Pasadena, Calif. : California Institute of Technology, 1994. http://resolver.caltech.edu/CaltechETD:etd-09172008-085430.

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Tout, Christopher Adam. "Binary stars and mass loss." Thesis, University of Cambridge, 1989. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.316766.

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Prieto, Jose L. "Massive Stars: Life and Death." The Ohio State University, 2009. http://rave.ohiolink.edu/etdc/view?acc_num=osu1248987393.

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Burnley, Adam Warwick. "Mass loss from hot, luminous stars." Thesis, University College London (University of London), 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.408417.

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Viviers, Etienne. "Lost in the stars Kurt Weill and Maxwell Anderson's musical adaptation of Alan Paton's novel Cry the beloved country /." Diss., Pretoria : [s.n.], 2008. http://upetd.up.ac.za/thesis/available/etd-11252008-142122/.

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Oskinova, Lidia M., Richard Ignace, and D. P. Huenemoerder. "X-ray Diagnostics of Massive Star Winds." Digital Commons @ East Tennessee State University, 2016. https://dc.etsu.edu/etsu-works/2703.

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Observations with powerful X-ray telescopes, such as XMM-Newton and Chandra, significantly advance our understanding of massive stars. Nearly all early-type stars are X-ray sources. Studies of their X-ray emission provide important diagnostics of stellar winds. High-resolution X-ray spectra of O-type stars are well explained when stellar wind clumping is taking into account, providing further support to a modern picture of stellar winds as non-stationary, inhomogeneous outflows. X-ray variability is detected from such winds, on time scales likely associated with stellar rotation. High-resolution X-ray spectroscopy indicates that the winds of late O-type stars are predominantly in a hot phase. Consequently, X-rays provide the best observational window to study these winds. X-ray spectroscopy of evolved, Wolf-Rayet type, stars allows to probe their powerful metal enhanced winds, while the mechanisms responsible for the X-ray emission of these stars are not yet understood.
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Coté, Jacqueline. "Formation and mass loss of be stars." Amsterdam : Amsterdam : Sterrenkundig Instituut " Anton Pannekoek" ; Universiteit van Amsterdam [Host], 1993. http://dare.uva.nl/document/91638.

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Smith, Nathan, Jose H. Groh, Kevin France, and Richard McCray. "Ultraviolet spectroscopy of the blue supergiant SBW1: the remarkably weak wind of a SN 1987A analogue." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/624061.

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The Galactic blue supergiant SBW1 with its circumstellar ring nebula represents the best known analogue of the progenitor of SN 1987A. High-resolution imaging has shown H alpha and infrared structures arising in an ionized flow that partly fills the ring's interior. To constrain the influence of the stellar wind on this structure, we obtained an ultraviolet (UV) spectrum of the central star of SBW1 with the Hubble Space Telescope Cosmic Origins Spectrograph. The UV spectrum shows none of the typical wind signatures, indicating a very low mass-loss rate. Radiative transfer models suggest an extremely low rate below 10(-10) M-circle dot yr(-1), although we find that cooling time-scales probably become comparable to (or longer than) the flow time below 10(-8) M-circle dot yr(-1). We therefore adopt this latter value as a conservative upper limit. For the central star, the model yields T-eff = 21 000 +/- 1000 K, log(g(eff)) = 3.0, L similar or equal to 5 x 10(4) L-circle dot, and roughly Solar composition except for enhanced N abundance. SBW1' s very low mass-loss rate may hinder the wind's ability to shape its nebula and to shed angular momentum. The spin-down time-scale for magnetic breaking is more than 500 times longer than the age of the ring. This, combined with the star's slow rotation rate, constrains merger scenarios to form ring nebulae. The mass-loss rate is at least 10 times lower than expected from mass-loss recipes, without any account of clumping. The physical explanation for why SBW1' s wind is so weak presents an interesting mystery.
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Young, Patrick Allen. "Hydrodynamics, nucleosynthesis, and mass loss in massive stars." Diss., The University of Arizona, 2004. http://hdl.handle.net/10150/280579.

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I test the predictive power of the stellar evolution code TYCHO. Systematic errors are present in the predictions for double-lined eclipsing binary stars when only standard physics common to the majority of stellar evolution codes is included. A mechanism for driving slow circulation and mixing in the radiative regions of stars is identified in numerical simulations of convection and a physical theory developed. Mixing is caused by dissipation of inertial waves driven by the interaction of convective fluid motions with the boundary of the convection zone. Evolutionary calculations incorporating this physics are tested in several observational regimes. Light element depletion in young clusters, turnoff ages of young clusters with brown dwarf Li depletion ages, and evolution of carbon stars on the asymptotic giant branch are all predicted satisfactorily. Tests of solar models yield good agreement with surface observables, chemical abundances, helioseismological data, and neutrino fluxes. The predictive accuracy of a non-calibrated, state-of-the-art stellar evolution code is ∼7% for surface observables. The main sequence sun is relatively easy to model, so this gives an estimate of our minimum predictive error. The solar models also highlight problems with uniqueness of evolutionary tracks converging on a given point and the potential for avoiding the effects of missing physics by calibration. A reanalysis of the binary sample with the more complete physics shows a dramatic improvement in the accuracy of the models. The potential for avoiding the effects of missing physics by calibration is explored. A TYCHO model for a late AGB star is used for the boundary conditions on a hydrodynamic simulation of proto-planetary nebula evolution as an illustration of the unified technique. NaCl and NaCn are observed at large radii in the Egg Nebula. These molecules require high densities to form, which are difficult to explain at large distances from the star. The 2-D simulation of a fast wind interacting with earlier mass loss produces clumps of material through a thermal instability with the necessary conditions for formation of the molecules. In conclusion, the effects of the more complete physics on the core size and abundance profiles of a massive star during core Si burning are examined as an example of future developments.
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Ignace, Richard. "Long-Wavelength, Free–Free Spectral Energy Distributions from Porous Stellar Winds." Digital Commons @ East Tennessee State University, 2016. https://dc.etsu.edu/etsu-works/2685.

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The influence of macroclumps for free–free spectral energy distributions (SEDs) of ionized winds is considered. The goal is to emphasize distinctions between microclumping and macroclumping effects. Microclumping can alter SED slopes and flux levels if the volume filling factor of the clumps varies with radius; however, the modifications are independent of the clump geometry. To what extent does macroclumping alter SED slopes and flux levels? In addressing the question, two specific types of macroclump geometries are explored: shell fragments (pancake-shaped) and spherical clumps. Analytic and semi-analytic results are derived in the limiting case that clumps never obscure one another. Numerical calculations based on a porosity formalism is used when clumps do overlap. Under the assumptions of a constant expansion, isothermal, and fixed ionization wind, the fragment model leads to results that are essentially identical to the microclumping result. Mass-loss rate determinations are not affected by porosity effects for shell fragments. By contrast, spherical clumps can lead to a reduction in long-wavelength fluxes, but the reductions are only significant for extreme volume filling factors.
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Books on the topic "Lost in the stars"

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Tracing stars. New York: Philomel Books, 2012.

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The lost stars: Tarnished knight. New York: Penguin Group, 2012.

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Aligay saves the stars. New York: Scholastic Inc., 1991.

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Stone, Kazuko G. Aligay saves the stars. New York: Scholastic Inc., 1991.

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Stars screaming. New York: Atlantic Monthly Press, 1997.

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Goble, Paul. The lost children: The boys who were neglected. New York: Bradbury Press, 1993.

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Goble, Paul. The lost children: The boys who were neglected. New York: Bradbury Press, 1993.

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Rachel, Connolly, ed. Lost in space: Everything you wanted to know about planets, stars, galaxies, and beyond. New York: Scholastic, 2007.

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The sun and other stars. New York: Simon & Schuster, 2014.

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The sun and other stars. Waterville, Maine: Thorndike Press, 2014.

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Book chapters on the topic "Lost in the stars"

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Turney, Chris. "The Lost Worlds." In Bones, Rocks and Stars, 104–18. New York: Palgrave Macmillan US, 2006. http://dx.doi.org/10.1007/978-0-230-55230-2_9.

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Kelly, Gillian. "Robert Taylor: The ‘Lost’ Star with the Long Career." In Lasting Screen Stars, 85–98. London: Palgrave Macmillan UK, 2016. http://dx.doi.org/10.1057/978-1-137-40733-7_7.

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Portmann, John. "Stunning stars." In Celebrity Morals and the Loss of Religious Authority, 25–43. Abingdon, Oxon ; New York : Routledge, 2019. | Series: Routledge studies in religion: Routledge, 2019. http://dx.doi.org/10.4324/9780429273469-3.

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O’Ceallaigh Ritschel, Nelson. "The Plough and the Stars: The Lost Workers’ Republic." In Bernard Shaw and His Contemporaries, 189–229. Cham: Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-74274-4_6.

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Hughes, V. A. "Mass-Loss During the Star Forming Process in Cep A." In Radio Stars, 155–58. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5420-5_24.

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Cassinelli, Joseph P. "Mass loss from stars." In The Century of Space Science, 895–911. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0320-9_39.

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De Freitas Pacheco, J. A. "Mass Loss Rates from B[e] Stars." In B[e] Stars, 221–25. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-015-9014-3_24.

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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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Dupree, A. K., and D. Reimers. "Mass Loss from Cool Stars." In Astrophysics and Space Science Library, 321–53. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3753-6_14.

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Zuckerman, B. "Mass Loss by Cool Stars." In Light on Dark Matter, 93–100. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4672-9_19.

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Conference papers on the topic "Lost in the stars"

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Krtička, J., and J. Kubát. "The Mass Loss from Hot Pop III Stars." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905556.

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Muijres, L., and A. de Koter. "The Effect of Clumping on Predictions of the Mass‐Loss Rate of Early‐Type Stars." In FIRST STARS III: First Stars II Conference. American Institute of Physics, 2008. http://dx.doi.org/10.1063/1.2905543.

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Puls, J., J. O. Sundqvist, F. Najarro, M. M. Hanson, Ivan Hubeny, James M. Stone, Keith MacGregor, and Klaus Werner. "Mass loss from OB-stars." In RECENT DIRECTIONS IN ASTROPHYSICAL QUANTITATIVE SPECTROSCOPY AND RADIATION HYDRODYNAMICS: Proceedings of the International Conference in Honor of Dimitri Mihalas for His Lifetime Scientific Contributions on the Occasion of His 70th Birthday. AIP, 2009. http://dx.doi.org/10.1063/1.3250053.

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Tabatabaei, Maryam, and Arash Dahi Taleghani. "Smart Lost Circulation Materials to Seal Large Fractures." In SPE Annual Technical Conference and Exhibition. SPE, 2021. http://dx.doi.org/10.2118/205873-ms.

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Abstract Lost circulation problems may result in a significant downtime, a considerable reduction of the rate of penetration, or even well control problems. Despite advances in manufacturing lost circulation materials (LCMs), some formations, like heavily fractured carbonates, have complete losses during drilling. We develop smart LCMs using shape memory polymers (SMPs), and program them thermo-mechanically to satisfy size limitations imposed by bottomhole assemblies (BHA). Elevated downhole temperatures act as an external trigger to recover the permanent shape of LCMs, which could expand ten times larger than the temporary (programmed) dimensions for deployment. Smart LCMs are a combination of various material categories such as granular, fibrous (one-dimensional or 1-D) and planar (two-dimensional or 2-D) configurations that resume to the original shape after exposure to high temperatures. The LCMs form different structures such as flatted pellet, disc-shaped, spider-shaped, and spindled, which, respectively, presents grains, 1-D fibers, 2-D stars, and 2-D lattices after recovery. A combination of the above categories attempt to build three-dimensional (3-D) plugging capabilities across various sized fractures.
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Vink, Jorick S., Richard J. Stancliffe, Guenter Houdek, Rebecca G. Martin, and Christopher A. Tout. "Mass-loss Predictions for Hot Stars." In UNSOLVED PROBLEMS IN STELLAR PHYSICS: A Conference in Honor of Douglas Gough. AIP, 2007. http://dx.doi.org/10.1063/1.2818998.

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Ge, Hongwei, Ronald F. Webbink, Xuefei Chen, Zhanwen Han, Vicky Kologera, and Marc van der Sluys. "Stellar Adiabatic Mass Loss in Binary Stars." In INTERNATIONAL CONFERENCE ON BINARIES: In celebration of Ron Webbink’s 65th Birthday. AIP, 2010. http://dx.doi.org/10.1063/1.3536410.

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Chesneau, Olivier. "The asymmetric mass-loss of evolved stars." In SPIE Astronomical Telescopes + Instrumentation. SPIE, 2008. http://dx.doi.org/10.1117/12.789760.

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Hirschi, Raphael, Cristina Chiappini, Georges Meynet, Sylvia Ekström, André Maeder, Richard J. Stancliffe, Guenter Houdek, Rebecca G. Martin, and Christopher A. Tout. "Mass Loss and Very Low-metallicity Stars." In UNSOLVED PROBLEMS IN STELLAR PHYSICS: A Conference in Honor of Douglas Gough. AIP, 2007. http://dx.doi.org/10.1063/1.2818999.

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Wood, P. R., Richard J. Stancliffe, Guenter Houdek, Rebecca G. Martin, and Christopher A. Tout. "Mass Loss from Low- and Intermediate-mass Stars." In UNSOLVED PROBLEMS IN STELLAR PHYSICS: A Conference in Honor of Douglas Gough. AIP, 2007. http://dx.doi.org/10.1063/1.2818991.

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Deval Samirbhai, Mehta, Yan Wending, and Shoushun Chen. "A star shortlisting technique for a lost-in-space mode star tracker." In 2018 IEEE Aerospace Conference. IEEE, 2018. http://dx.doi.org/10.1109/aero.2018.8396398.

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Reports on the topic "Lost in the stars"

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Grassi, F. Quark core stars, quark stars and strange stars. Office of Scientific and Technical Information (OSTI), January 1988. http://dx.doi.org/10.2172/5237159.

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Gutiérrez, Germán, and Thomas Philippon. Fading Stars. Cambridge, MA: National Bureau of Economic Research, February 2019. http://dx.doi.org/10.3386/w25529.

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Hernandez, Rhett. Lost Priorities. Fort Belvoir, VA: Defense Technical Information Center, January 1998. http://dx.doi.org/10.21236/ada442002.

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Agrawal, Ajay, John McHale, and Alex Oettl. Why Stars Matter. Cambridge, MA: National Bureau of Economic Research, March 2014. http://dx.doi.org/10.3386/w20012.

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Ekman, R. STARS Reusability Guidelines. Fort Belvoir, VA: Defense Technical Information Center, April 1990. http://dx.doi.org/10.21236/ada228468.

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Martin, Ian W. R., and Robert Pindyck. Welfare Costs of Catastrophes: Lost Consumption and Lost Lives. Cambridge, MA: National Bureau of Economic Research, July 2019. http://dx.doi.org/10.3386/w26068.

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Palmisano, Danielle. Lost in Beauty. Ames: Iowa State University, Digital Repository, February 2013. http://dx.doi.org/10.31274/itaa_proceedings-180814-590.

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Eggleton, P. Magnetic Dynamos and Stars. Office of Scientific and Technical Information (OSTI), February 2007. http://dx.doi.org/10.2172/1036872.

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Ekman, R. IBM STARS Repository Guidebook. Fort Belvoir, VA: Defense Technical Information Center, April 1990. http://dx.doi.org/10.21236/ada228470.

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Murray, Craig H. Gallipoli 1915-Opportunity Lost? Fort Belvoir, VA: Defense Technical Information Center, May 1994. http://dx.doi.org/10.21236/ada283403.

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