Relevant bibliographies by topics / Intersteller hydrogen

Academic literature on the topic 'Intersteller hydrogen'

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Published: 10 December 2022
Last updated: 28 January 2023

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Journal articles on the topic "Intersteller hydrogen"

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Lin, Ching Yeh, Andrew T. B. Gilbert, and Mark A. Walker. "INTERSTELLAR SOLID HYDROGEN." Astrophysical Journal 736, no. 2 (July 12, 2011): 91. http://dx.doi.org/10.1088/0004-637x/736/2/91.

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Etim, Emmanuel E., Prasanta Gorai, Ankan Das, Sandip K. Chakrabarti, and Elangannan Arunan. "Interstellar hydrogen bonding." Advances in Space Research 61, no. 11 (June 2018): 2870–80. http://dx.doi.org/10.1016/j.asr.2018.03.003.

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Whang, Y. C. "Ionization of Interstellar Hydrogen." Astrophysical Journal 468 (September 1996): 947. http://dx.doi.org/10.1086/177749.

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Shull, J. Michael. "Observing interstellar molecular hydrogen." Physics Today 75, no. 12 (December 1, 2022): 12. http://dx.doi.org/10.1063/pt.3.5132.

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Balm, S. P., and H. W. Kroto. "Possible assignment of the 11.3-μm UIR feature to emission from carbonaceous microparticles with internal hydrogens." Monthly Notices of the Royal Astronomical Society 245, no. 2 (July 15, 1990): 193. http://dx.doi.org/10.1093/mnras/245.2.193.

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Summary The carriers of the UIR bands seen in many galactic and extragalactic objects have previously been assigned to emission from polycyclic aromatic hydrocarbons (PAHs). However, the match between laboratory spectra of typical PAHs with the interstellar features in the structurally sensitive 11-15-μm (909-667-cm-1) region remains unsatisfactory. In particular, it has been difficult to explain, considering that a PAH mixture is undoubtedly involved, why only one strong band is seen at 11.3 μm (885 cm-1) and why this has the same position in all sources. We discuss here the possibility that a hitherto unrecognized class of molecule containing a novel type of hydrogen functional group, the internal hydrogen, may provide important new clues to the origin of the 11.3-μm (885 cm-1) feature. This type of grouping is typified by the molecule kekulene which contains six such internal hydrogens and exhibits bands in its IR absorption spectrum which coincide with the interstellar feature. This structural unit is likely to be common in soot-like microparticles which simulations suggest are present in the cool carbon-rich outflows of red giant stars and hence should contribute to the 11.3-μm (885-cm-1) emission.
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Neufeld, David A., and Sheldon Green. "Excitation of interstellar hydrogen chloride." Astrophysical Journal 432 (September 1994): 158. http://dx.doi.org/10.1086/174557.

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Bergman, P., B. Parise, R. Liseau, B. Larsson, H. Olofsson, K. M. Menten, and R. Güsten. "Detection of interstellar hydrogen peroxide." Astronomy & Astrophysics 531 (June 20, 2011): L8. http://dx.doi.org/10.1051/0004-6361/201117170.

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Neufeld, David A., Jonas Zmuidzinas, Peter Schilke, and Thomas G. Phillips. "Discovery of Interstellar Hydrogen Fluoride." Astrophysical Journal 488, no. 2 (October 20, 1997): L141—L144. http://dx.doi.org/10.1086/310942.

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Irvine, William M. "Microwave Spectroscopy of Astrophysical Molecules." Highlights of Astronomy 8 (1989): 339–44. http://dx.doi.org/10.1017/s1539299600007966.

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ABSTRACTRecent detections of new molecules in dense interstellar clouds, first detections of certain chemical elements in interstellar molecules, and new information on isotopic fractionation of hydrogen in the interstellar medium are discussed in the context of the need for new laboratory data on transition rest frequencies, reaction rates, and branching ratios.
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Prieto, Jorge Enrique Bueno. "PP - Organic synthesis of uracil from interstellar organic molecules." Proceedings of the International Astronomical Union 4, S251 (February 2008): 475–76. http://dx.doi.org/10.1017/s1743921308022217.

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AbstractIt is important to say that the formaldehyde and hydrogen cyanide have been detected in the interstellar medium through resonance spectrum emission. Here I describe a way to produce uracil in interstellar space.
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Dissertations / Theses on the topic "Intersteller hydrogen"

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Malawi, Abdulrahman Ali. "Atomic hydrogen associated with high latitude IRAS cirrus clouds." Thesis, University of Manchester, 1989. https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.664465.

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Islam, F. "The formation of molecular hydrogen in the interstellar medium." Thesis, University College London (University of London), 2010. http://discovery.ucl.ac.uk/19475/.

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H2 is the most abundant molecule in the interstellar medium and forms on the surface of interstellar dust grains. Laboratory studies have been conducted of HD formation on a dust grain analogue, which is a highly-oriented pyrolytic graphite surface held at 15 K, under ultra-high vacuum. The molecules desorb from the surface in a distribution of ro-vibrational states, which are probed using Resonance Enhanced Multi-Photon Ionization Spectroscopy. HD in a particular ro-vibrational state is ionized using laser photons detected by a time-of-flight mass spectrometer. The HD+ ion yields are then data processed to obtain the relative rotational populations of HD formed within one vibrational level and an average rotational temperature can be found. In this thesis, HD formed in vibrational states v = 3 – 7 have been studied. This carries on from previous studies of HD and H2 in the v = 1 and 2 states. Within each vibrational level, the most populated rotational state was found to be J = 1 or 2. The most populated vibrational state was found to be v = 4. The HD experimental results were extrapolated to give the relative ro-vibrational population distribution of nascent H2, which provides a new model for the formation pumping of H2. This new formation pumping model has been implemented into a radiative transfer code, written by Casu and Cecchi-Pestellini, which takes into account formation, radiative and collisional pumping mechanisms to calculate the total population distribution of H2 in an interstellar cloud and to generate H2 spectra. The sensitivity of the H2 spectra to the physical conditions of interstellar dark clouds, such as cloud density and temperature, has been investigated. H2 spectra generated using the new experimentally-derived formation pumping model has also been compared to H2 spectra generated using other established, theoretically-derived formation pumping models.
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Irving, Benjamin James. "The formation of molecular hydrogen in the interstellar medium." Thesis, University of Sheffield, 2012. http://etheses.whiterose.ac.uk/3104/.

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Kreckel, Holger. "Internal excitations of stored triatomic hydrogen molecular ions." [S.l. : s.n.], 2003. http://deposit.ddb.de/cgi-bin/dokserv?idn=968519563.

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Burton, Michael Graham. "The shock-excitation of molecular hydrogen in the interstellar medium." Thesis, University of Edinburgh, 1987. http://hdl.handle.net/1842/855.

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This dissertation presents a study of shock-excited molecular hydrogen (H2) in the interstellar medium. The aims of this thesis are to understand the shock-excitation process and to understand the global role of shocks in the interstellar medium. These aims are quantified as the investigation of specific problems. To address the problems, a variety of observing techniques have been applied and several sources studied, with particular reference on supernova remnant IC 443. An analytical model for the cooling flow behind a shock has also been developed. The observations show that extensive regions of low surface brightness H2 line emission are common in shocked molecular sources. Models are presented for three sources; IC 443, CRL 616 and OMC-1. In IC 443 emission comes from a sinuous ridge, about 20 parsecs long ans less than a parsec wide, with over 20 bright emission peaks distributed along it. The total H2 line luminosity is ~1600L, making IC 443 one of the brightest galactic H2 emission line objects yet detected. The spatial distributions of accelerated line emissions from other molecules (CO, HCO+, HCN) and atomic gas (HI) are remarkably similar to that of shocked H2. There is evidence for partial dissociation of molecular gas by the shock, but there can be little ionised gas present. Important cooling mechanisms for the hot gas (and possibly the dominant mechanisms) are H2 line radiation and H2 dissociation, except possibly in the densest clumps where far-IR emission from collisionally heated grains may dominate. H" line profiles were obtained in several sources and show considerable variation between sources. In CRL 618 the line is ~250km/s wide, the largest yet measured for a galactic source, and is composed of several discrete components. the high-velocity line emission is interpreted as being due to the shocking of high-velocity, discrete molecular clumps, embedded in and shocked by a stellar wind. Line polarization measurements in OMC-1 show there are two distinct regions of H2 line emission. In the outflow region the line is dichroically polarized by a slab of alligned grains lying between us and the outflow, with polarization vectors parallel to the outflow axis. The alignment mechanism is possibly due to the agency of a magnetic field, and thus the polarization vectors may trace the magnetic field direction which is therefore aligned with the outflow axis. Outside the core region the polarization vectors show a centro-symmetric pattern characteristic of scattering, centred on the region of peak molecular hydrogen emission. This amounts to the discovery of a molecular hydrogen reflection nebula. Observations of five H2 lines, in four types of sources, show no major differences in relative line ratios between sources. This is dispite different pre-shock conditions being expected in each source. The shocked gas cannot be characterised by a single excitation temperature. An analytical model has been developed for the cooling flow behind a jump-shock into molecular gas, driven by an isobaric thermal pressure. The model predicts that, when the density is larger than the critical density needed to thermalise the level populations of the dominant coolant, and t the post-shock temperature is sufficiently large, then the line ratios only depend on the upper-state level energies of the lines and on the form of the cooling function. For the observed excitation temperatures, the dominant cooling mechanism, consistent with the data, is cooling through the vibrational/ rotational lines of the hydrogen molecule itself. This conclusion applies when the temperature is in the range ~500 - 4000 K and the gas density is >10(5)cm-3
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Ward, M. D. "Reactions of hydrogen and oxygen atoms on interstellar grain analogues." Thesis, University College London (University of London), 2012. http://discovery.ucl.ac.uk/1355953/.

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The region of space between stars, the interstellar medium, has been found to contain over 160 chemical species to date. These molecules are contained within regions of gas and dust, measuring several light years across, known as interstellar dust clouds. Many of these molecular species are formed in the gas phase, for example, via the reactions of molecules with ions. However, some critical gas phase processes are often slow due to the low temperatures and pressures found in the interstellar medium and cannot readily account for the abundances of some species. Consequently reactions on the surfaces of interstellar dust grains are often invoked to explain the abundances some molecules. These dust grains represent approximately 1 % of the mass of a typical interstellar dust cloud and typically consist of carbon, silicates or metal oxides. The temperature of these interstellar dust grains is low enough (~ 10 K) that over time icy mantles consisting of simple atomic and molecular species can build up on their surfaces. Whether and how these simple species can be processed to form more complex molecules such as alcohols, simple sugars and potentially amino acids is a key astrochemical problem. One way in which astrophysical ices can be processed to form more complex species is via the reactions of species within the ice with simple free radicals such as H, C, N and O. This thesis therefore presents experimental studies of the reactions of atomic species with some astrophysically relevant molecular ices under interstellar conditions. Since hydrogen and oxygen are the first and third most abundant elements in the interstellar medium respectively, these experiments have specifically focussed upon the reactions of hydrogen and oxygen atoms. In addition to the characterization of surface reactions between key astrochemical species, kinetic parameters for use in astrochemical models are derived from these experiments.
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Richter, Philipp. "FUV absorption spectroscopy of interstellar molecular hydrogen towards the Magellanic clouds /." Aachen : Shaker, 1999. http://catalogue.bnf.fr/ark:/12148/cb37739235j.

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Dissertation--Mathematisch-Naturwissenschaftliche Fakultät--Bonn--Rheinische Friedrich-Wilhelms-Universität, 1999. Titre de soutenance : FUV spectroscopy of interstellar molecular hydrogen towards the Magellanic clouds.
FUV = far ultraviolet. Bibliogr. p. 83-85.
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Gaylard, Michael John. "Radio studies of ionized hydrogen in the southern Milky Way." Thesis, Rhodes University, 1990. http://hdl.handle.net/10962/d1001993.

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This thesis describes the results of a survey of the HI42ɑ recombination line emission at 2.3 GHz from HII regions in the Southern Milky Way, carried out with the 26 m diameter Hartebeesthoek radio telescope. The Galactic Longitude range covered was 290° to 40°. Single recombination lines were detected from 375 positions. Multiple lines were observed towards 90 positions in the inner Galaxy. No line emission could be detected in 28 positions. Continuum antenna temperatures were estimated from drift scans or radio maps observed for the purpose. LTE electron temperatures and turbulent velocities of the HII regions were calculated where possible. The properties of the sample were compared to those observed in HI09ɑ surveys. The lines observed from over 50 positions were first detections, of which half were associated with optically-identified HII regions. In about 150 cases the lines were only the second to be detected from those HII regions. The processes of the radio emission, detection, and analysis were simulated numerically. The detectability of the emission and the magnitude of non-LTE effects and pressure-broadening in multi-component HII regions was predicted and compared to observations. The radio luminosity function of the HII regions was determined over a range of three orders of magnitude in intrinsic brightness for the first time, using techniques which corrected for different types of incompleteness in the samples. The luminosity function was compared to those in five selected spiral galaxies, and shown to lie between those of M33 and M81. An alternate form of the luminosity function was developed for use with a numerical model of the spiral arm structure of the Milky Way. The physical parameters defining the major spiral arms were established by comparing synthesized diagrams of radial velocity versus Galactic Longitude with those actually observed. The faint, extended HII regions S9 and RCW129 in Scorpius, the Barnard Loop in Orion, and S296 in Canis Major were analyzed, using all available data. All the recombination lines from these HII regions were first detections
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Gavilan, Lisseth. "The formation of molecular hydrogen on interstellar silicatesé : from experiments to observations." Observatoire de Paris, 2013. https://hal.science/tel-02095146.

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L'objectif de cette thèse est de comprendre la formation de l'hydrogène moléculaire dans le milieu interstellaire (MIS) via des expériences de laboratoire et des observations astronomiques. Les expériences ont été réalisées avec FORMOLISM, un montage fonctionnant dans l'ultra-vide pour étudier la formation de molécules dans le MIS. On s'intéresse à la distribution en énergie de molécules d'hydrogène formées sur une surface refroidie par cryogénie (< 10 K). La technique de Resonance Enhanced Multi-Photon Ionization (REMPI 2 + 1) est utilisée pour sonder la population des niveaux rovibrationnels de l'état électronique fondamental de l'hydrogène moléculaire. Nous avons examiné différentes surfaces d'intérêt astrophysique : des silicates amorphes et cristallins, et de la glace d'eau solide amorphe poreuse (p-ASW). Nous avons confirmé l'augmentation du taux de formation de l'hydrogène moléculaire sur une surface recouverte au préalable des molécules d'hydrogène et nous avons quantifié la formation D₂en tant que mécanisme de désorption non-thermique. Nous avons mesuré le rapport ortho-para de l'hydrogène moléculaire nouvellement formée sur la surface de p-ASW, qui correspond à la valeur attendue à l'équilibre statistique à haute température (> 100 K). Nous avons fabriqué au laboratoire de nouvelles surfaces de silicates (forstérite et fayalite) pour examiner l'impact de leur morphologie et de leur composition chimique sur la formation de l'hydrogène moléculaire. On a observé l'abaissement de la température de rotation des molécules d'hydrogène formées (par rapport à la température de rotation du jet moléculaire) émergeant de surfaces cristallines. Nous avons également étudié la conversion de spin nucléaire des molécules d'hydrogène absorbées sur une surface de sillicate. Les prédictions observationnelles qui on été déduites de ces expériences ont été testées par spectroscopie à longue fente dans l'infrarouge proche disponible au VLT et au Keck. Des nébuleuses planétaires présentant simultanément des émissions de H₂ont été détectées sur certains de nos objets. La distribution d'intensité de ces raies est comparée à des modèles théoriques de formation H₂dans l'espace. Une partie de cette thèse traite également de la spectroscopie VUV à haute résolution de CO et de ses isotopes, en utilisant le spectromètre à transformée de Fourier disponible au synchroton SOLEIL. Cela complète le travail sur l'hydrogène dans le contexte plus large de l'astrochimie de petites molécules
The goal of this thesis is to understand the formation of molecular hydrogen in the interstellar medium (ISM) via laboratory experiments and astronomical observations. The experiments are performed with FORMOLISM, an ultra-high vacuum setup to study the formation of molecules in the ISM. We are interested in the energy disposal during the exhothermic recombination of two H atoms on a cryogenically cooled surface (< 10 K). Resonance Enhanced Multi-Photon Ionization ( REMPI 2 + 1) spectroscopy is used to probe the population of rovibrational levels in the ground electronic state of molecular hydrogen after formation. We have tested different surfaces of astrophysical relevance : amorphous and crystalline silicates, porous amorphous solid water, and a bare silicate pre-dosed with hydrogen molecules. We have confirmed the formation enhancement of molecular hydrogen on a surface pre-dosed with molecules and quantified D₂formation as a non-thermal desorption mechanism. We have also measured the ortho-to-para ratio of newly formed molecular hydrogen on p-ASW, finding that it corresponds to the value expected at statistical equilibrium at high temperature. Silicate analog surfaces (forsterite and fayalite) have been fabricated to test the influence of their morphology and chemical composition on hydrogen formation. We have found that newly formed molecular hydrogen leaves rotationally cooler (with respect to the molecular beam rotational temperature) from crystalline surfaces, and that it is unaffected when it scatters from amorphous surfaces. We have also detected nuclear spin conversion of molecular hydrogen absorbed on bare silicates. Observational predictions from these experiments are tested using long slit near infrared spectroscopy available at the VLT and Keck telescopes. Planetary nebulae with H₂ and X-ray emission were chosen as ideal targets. H₂transitions have been detected throughout our targets. The intensity distribution of these transitions will be compared to models of formation pumping spectra. In addition, part of this thesis addresses the VUV high-resolution spectroscopy of CO and its isotopologues, using the Fourier Transform Spectrometer at the SOLEIL synchroton. This complements the work on hydrogen in the wider context of the astrochemistry of small molecules
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Kulesa, Craig A. "Molecular hydrogen and its ions in dark interstellar clouds and star forming regions." Diss., The University of Arizona, 2002. http://hdl.handle.net/10150/280192.

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Fundamental observations of molecular hydrogen (H₂) in dark clouds, star forming regions, and radiation-dominated environments are presented, modeled, and interpreted. Through a weak infrared absorption line spectrum, the abundance of cold H₂ in dark molecular clouds and star forming regions is measured directly and compared with the abundance of its most commonly cited surrogate, CO. The derived abundance of CO is between 1.5 and 2.5 x 10⁻⁴ for the sample. The CO molecule thus represents about ⅓ of the total carbon budget in dense clouds. Also detected via infrared line absorption is the pivotal molecular ion H⁺₃ , yielding a direct measure of the cosmic ray ionization rate of H₂ in dark molecular clouds (between 1 and 5 x 10⁻¹⁷ s⁻¹), a process that instigates the complex ion-neutral chemical pathways that form many of the 120+ known molecular species deep inside interstellar clouds. These timely tests of theory are applied to the detailed submillimeter-wave study of the ρ Ophiuchi star forming cloud and photodissociation front, allowing partial disentanglement of the complicated physical and chemical structure of a star forming cloud. Yet H₂ and H⁺₃ continue to surprise and delight us with more mysteries. The formation, excitation and survival of molecules in unusual & hostile environments is highlighted by the discoveries of H⁺₃ in circumstellar disks of early-type stars, and of fluorescing H₂ in two harshly-irradiated filaments of the Crab Nebula. The role of H⁺₃ as a possible tracer of planet formation, and the evolution of H₂ in the interstellar medium is discussed. The study of H₂ in hostile environments is extended to the ensemble properties of extragalactic star forming regions, and applied to the Arp 299 merger system as a unique probe of the feedback of newly-formed hot stars, their fossil remains, and the molecular material which formed them.
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Books on the topic "Intersteller hydrogen"

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1940-, Burton W. B., ed. Atlas of galactic neutral hydrogen. Cambridge: Cambridge University Press, 1997.

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Hartmann, Dap. The Leiden/Dwingeloo survey of galactic neutral hydrogen. Leiden: Sterrewacht Leiden, 1995.

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Hartmann, Dap. The Leiden/Dwingeloo survey of galactic neutral hydrogen. Leiden: Sterrewacht Leiden, 1994.

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Searching for water in the universe. New York: Springer, 2007.

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Frail, Dale A. A study of the diffuse interstellar medium through neutral hydrogen absorption observations toward pulsars. Toronto: University of Toronto, Dept. of Astronomy, 1989.

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Molecular Hydrogen in Space. Cambridge University Press, 2001.

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Hartmann, Dap, and W. Butler Burton. Atlas of Galactic Neutral Hydrogen. Cambridge University Press, 2012.

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Combes, F., and G. Pineau des Forets. Molecular Hydrogen in Space. Cambridge University Press, 2012.

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Combes, F., and G. Pineau des Forets. Molecular Hydrogen in Space. Cambridge University Press, 2010.

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David, Skillman Evan, and University of Minnesota, eds. The Minnesota lectures on extragalactic neutral hydrogen: A series of lectures presented at the University of Minnesota, Minneapolis, Minnesota, from 27 March 1994 [i.e. 1995] to 2 June 1994 [i.e. 1995]. San Francisco, Calif: Astronomical Society of the Pacific, 1996.

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Book chapters on the topic "Intersteller hydrogen"

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Verschuur, Gerrit. "Interstellar Neutral Hydrogen." In Astronomers' Universe, 71–83. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-13422-2_6.

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Gatley, Ian, and Norio Kaifu. "Infrared Observations of Interstellar Molecular Hydrogen." In Astrochemistry, 153–66. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4774-0_27.

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Whang, Y. C. "Moment Equation Description of Interstellar Hydrogen." In The Heliosphere in the Local Interstellar Medium, 387–92. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-1782-8_39.

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Tielens, A. G. G. M., L. J. Allamandola, J. R. Barker, and M. Cohen. "The Hydrogen Coverage of Interstellar PAHs." In Polycyclic Aromatic Hydrocarbons and Astrophysics, 273–86. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-4776-4_23.

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Kulkarni, Shrinivas R., and Carl Heiles. "Neutral Hydrogen and the Diffuse Interstellar Medium." In Astronomy and Astrophysics Library, 95–153. New York, NY: Springer New York, 1988. http://dx.doi.org/10.1007/978-1-4612-3936-9_3.

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Dickey, John M. "Measuring Atomic Hydrogen Masses Using the 21-cm Line." In The Interstellar Medium in Galaxies, 473–82. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0595-5_19.

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Ruciński, Daniel, and M. Bzowski. "Modelling of the Interstellar Hydrogen Distribution in the Heliosphere." In The Heliosphere in the Local Interstellar Medium, 265–76. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-1782-8_28.

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Phillips, Timothy R., and Sheldon Green. "Excitation of Interstellar Water by Ortho-and Para-Hydrogen." In Circumstellar Matter 1994, 537–38. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0147-9_132.

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Lin, Jingsu, and Gianfranco Vidali. "Laboratory Investigations of Hydrogen Recombination Reactions on Interstellar Dust Grain Analogues." In The Cosmic Dust Connection, 323–32. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-011-5652-3_25.

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Verschuur, Gerrit L. "Interstellar Neutral Hydrogen Filaments at High Galactic Latitudes and the Bennett Pinch." In Plasma Astrophysics and Cosmology, 187–98. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0405-0_18.

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Conference papers on the topic "Intersteller hydrogen"

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Vidali, G., D. Jing, and J. He. "Hydrogen and water in the interstellar medium." In FIRST INTERNATIONAL CONFERENCE ON CHEMICAL EVOLUTION OF STAR FORMING REGION AND ORIGIN OF LIFE: Astrochem2012. AIP, 2013. http://dx.doi.org/10.1063/1.4812598.

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Izmodenov, Vladislav V., Rosine Lallement, and Yury G. Malama. "Heliospheric interface filtration of the interstellar hydrogen." In The solar wind nine conference. AIP, 1999. http://dx.doi.org/10.1063/1.58828.

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Medvedev, M. G., A. B. Ostrovskii, and A. I. Vasyunin. "Stochastic on-lattice simulation of H2 formation on interstellar grains." In Всероссийская с международным участием научная конференция студентов и молодых ученых, посвященная памяти Полины Евгеньевны Захаровой «Астрономия и исследование космического пространства». Ural University Press, 2021. http://dx.doi.org/10.15826/b978-5-7996-3229-8.10.

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We realized stochastic model evaluating efficency of recombination H2 in interstellar medium based on the approach of the continious-time random walk on two-dimentional lattice. This method allows to model inhomogeneous surfaces. We estimate recombination efficiensy as a function of model parameters. The influence of uncertainty of diffusion/desorption energy ratio on molecular hydrogen recombination was considered also.
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Pauls, H. L., G. P. Zank, and L. L. Williams. "Solar wind/local interstellar medium interaction including charge exchange with neutral hydrogen." In Proceedings of the eigth international solar wind conference: Solar wind eight. AIP, 1996. http://dx.doi.org/10.1063/1.51443.

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Green, James C., Patrick Jelinsky, and Stuart Bowyer. "The ratio of neutral helium to neutral hydrogen in the local interstellar medium." In Cosmic abundances of matter. AIP, 1989. http://dx.doi.org/10.1063/1.37979.

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Verschuur, G. L. "Further evidence for the critical ionization velocity signature in interstellar neutral hydrogen emission profiles." In The 33rd IEEE International Conference on Plasma Science, 2006. ICOPS 2006. IEEE Conference Record - Abstracts. IEEE, 2006. http://dx.doi.org/10.1109/plasma.2006.1707331.

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Amiaud, L., F. Dulieu, S. Baouche, J. H. Fillion, A. Momeni, and J. L. Lemaire. "Isotopic Segregation of Molecular Hydrogen on Water Ice Surface at Low Temperature: Importance for Interstellar Grain Chemistry." In ASTROCHEMISTRY: From Laboratory Studies to Astronomical Observations. AIP, 2006. http://dx.doi.org/10.1063/1.2359539.

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Franchini, Mariagrazia, Carlo Morossi, and G. Vladilo. "Determining interstellar hydrogen and deuterium column densities by means of the Lyman channel of the SPECTRUM UV Rowland spectrograph: a pre-launch feasibility study." In SPIE's 1996 International Symposium on Optical Science, Engineering, and Instrumentation, edited by Pierre Y. Bely and James B. Breckinridge. SPIE, 1996. http://dx.doi.org/10.1117/12.255103.

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Satonkin, N. A., A. B. Ostrovsky, K. Kalnin, G. S. Fedoseev, and A. I. Vasyunin. "Three-dimensional modeling of the formation of molecular hydrogen on the surface of an interstellar dust grain by the off-lattice Monte Carlo method." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.065.

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Haupa, Karolina, Yuan-Pern Lee, and Gyorgy Tarczay. "APPLICATIONS OF H-ATOM QUANTUM-DIFFUSION REACTIONS IN SOLID PARA-HYDROGEN TO ASTROCHEMICAL STUDIES: FINDING A MYSTERIOUS LINK BETWEEN INTERSTELLAR ISOCYANIC ACID [HNCO] AND FORMAMIDE [H2NC(O)H]." In 74th International Symposium on Molecular Spectroscopy. Urbana, Illinois: University of Illinois at Urbana-Champaign, 2019. http://dx.doi.org/10.15278/isms.2019.ta06.

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