Contributors

Baranov, Dimitry; Bhananker, Sanjay M.; Cartagena, Rafael; Cereda, Maurizio; Cladis, Franklyn P.; Cullen, Bruce F.; Davis, Peter J.; Dutton, Richard P.; Enany, Nader M.; Ertner, Robert A.; Fischer, Gregory W.; Grissom, Thomas E.; Hang, Jian; Hecker, James G.; Helgeson, Lars E.; Hepner, David L.; Hoover, Jason M.; Horák, Jiří; Kaplan, Joel A.; Kaye, Alan D.; Kelton, Tom; Lahlou, Salim; Levy, Richard J.; Littlewood, Keith E.; Lynch, James J.; McClung, Heather; McGoldrick, Kathryn E.; Mittnacht, Alexander J.C.; Muravchick, Stanley; Neligan, Patrick J.; Nemergut, Edward C.; Oliver, William C.; Passannante, Anthony N.; Reich, David L.; Rock, Peter A.; Roizen, Michael F.; Scarfo, Keith; Segal, Scott; Kodali, Bhavani Shankar; Shore‐Lesserson, Linda; Sieber, Frederick E.; Soliman, Doreen; Sutker, Patricia B.; Tetzlaff, John E.; Urban, Michael K.

doi:10.1016/b978-141602212-1.50001-9

Cited by 5 publications

(9 citation statements)

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“…The fitting procedure was separately done in each of the rapidity subdivisions under the requirement that the NMEs be strictly positive, and then the mean-square average of the fitted values was taken. Note that we used the results of a global fit for the entire charmonium family (including, in particular, χ cJ and ψ ′ states) [19] to properly calculate the feed-down contributions from h c , χ cJ , and ψ ′ decays. For some (yet unrecognized) reasons, our 1 P…”

Section: Numerical Resultsmentioning

confidence: 99%

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Prompt $$\eta _c$$ meson production at the LHC in the NRQCD with $$k_T$$-factorization

Baranov

Lipatov

2019

Eur. Phys. J. C

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In the framework of the kT -factorization approach, the prompt production of ηc mesons at the LHC conditions is studied. Our consideration is based on the off-shell amplitudes for hard partonic subprocesses and on the nonrelativistic QCD (NRQCD) formalism for the formation of bound states. We try two latest parametrizations for noncollinear, or transverse momentum dependent (TMD) gluon densities derived from the Catani-Ciafaloni-Fiorani-Marchesini (CCFM) equation. We use the values of the nonperturbative matrix elements obtained from a combined fit of the ηc and J/ψ differential cross sections. Finally, we show an universal set of parameters that provides a reasonable simultaneous description for all of the available data on the prompt J/ψ and ηc production at the LHC.

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Section: Numerical Resultsmentioning

confidence: 99%

“…contribution to η c production. In the forthcoming paper [19] we are going to present a global fit for the entire charmonium family, including J/ψ, χ cJ , ψ(2S) and η c mesons.…”

Section: Discussionmentioning

confidence: 99%

Prompt $$\eta _c$$ meson production at the LHC in the NRQCD with $$k_T$$-factorization

Baranov

Lipatov

2019

Eur. Phys. J. C

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“…Monte Carlo calculations have been performed using the same computational grid as described above for the plasma component. Since the TS and heliopause are the grid surfaces, we can define different populations of H atoms through their dependence on their place of origin (see, e.g., Malama 1991; Baranov et al 1998). Optimization of the critical weights in the Monte Carlo method has been performed separately for the each of the four populations (Malama 1990).…”

Section: Details Of the Numerical Scheme And Computational Gridmentioning

confidence: 99%

Three-Dimensional Kinetic-MHD Model of the Global Heliosphere With the Heliopause-Surface Fitting

Izmodenov

Alexashov

2015

ApJS

140

139

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This paper provides a detailed description of the latest version of our model of the solar wind (SW) interaction with the local interstellar medium (LISM). This model has already been applied to the analysis of Lyman-alpha absorption spectra toward nearby stars and for analyses of Solar and Heliospheric Observatory/SWAN data. Katushkina et al. (this issue) used the model results to analyze IBEX-Lo data. At the same time, the details of this model have not yet been pub-lished. This is a three-dimensional (3D) kinetic-magnetohydrodynamical (MHD) model that takes into account SW and interstellar plasmas (including α particles in SW and helium ions in LISM), the solar and interstellar magnetic fields, and the interstellar hydrogen atoms. The latitudinal dependence of SW and the actual flow direction of the interstellar gas with respect to the Sun are also taken into account in the model. It was very essential that our numerical code had been developed in such a way that any numerical diffusion or reconnection across the heliopause had not been allowed in the model. The heliospheric current sheet is a rotational discontinuity in the ideal MHD and can be treated kinematically. In the paper, we focus in particular on the effects of the heliospheric magnetic field and on the heliolatitudinal dependence of SW. Subject headings: Sun: heliosphere 1. Introduction Global modeling of the solar wind (SW) interaction with the local interstellar medium (LISM) is essential: (1) in general, to understand how the Sun acts as a star and exchanges matter and energy with the LISM, and (2) in particular, to explain relevant space experiment data (e.g. obtained on board of both Voyager spacecraft, the Interstellar Boundary Explorer (IBEX), the Solar and Heliospheric Observatory (SOHO), the Hubble Space Telescope (HST), etc.).Following the pioneering paper by Baranov & Malama (1993) self-consistent kinetic-gas dynamics models of the SW/LISM interaction were developed by our group in Moscow (e.g. Izmodenov and Baranov, 2006, Izmodenov et al., 2009, for reviews). There are two features which make our model approach different from similar models developed by other groups. These features are as follow: (1) a rigorous kinetic treatment of the interstellar H atom component using a Monte Carlo method with splitting of the trajectories, and (2) a Godunov-type numerical method used to solve the ideal gas dynamical or MHD equations. The method has the potential to fit some major discontinuities of the flow and to capture the others. The kinetic treatment of H atoms is essential because their mean free path is comparable to the size of the SW/LISM interaction region (see, e.g.,Izmodenov 2000). The difference between kinetic and alternative multi-component models has been explored in detail by Alexashov & Izmodenov (2005) and Müller et al. (2008). At the heliospheric distances smaller than 10-20 AU, solar gravitation and radiation forces make the kinetic effects even more important. The velocity distribution function of H atoms is essentially non-Max...

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“…As shown in Figure 1, this interaction results in a large scale structure for the heliosphere that consists of three boundaries: the termination shock (TS), where the solar wind is shocked to subsonic speeds; the bow shock (BS), where the ISM flow is shocked to subsonic speeds; and in between the two the heliopause (HP), which separates the plasma flows of the fully ionized solar wind and partially ionized ISM. Reviews of the history of heliospheric modeling include Holzer (1989), Baranov (1990), Zank (1999), and Baranov & Izmodenov (2006).…”

Section: Introductionmentioning

confidence: 99%

Dependence of Heliospheric Lyα Absorption on the Interstellar Magnetic Field

Wood

Izmodenov

Linsky

et al. 2007

ApJ

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We use newly developed 3D kinetic MHD models of the heliosphere to predict heliospheric H I Lyα absorption for various lines of sight. These predictions are compared with actual Lyα spectra from the Hubble Space Telescope, many of which have yielded previous detections of heliospheric absorption. We find that the absorption predicted by the models is weakly affected by both the magnitude and orientation of the assumed ISM magnetic field. Models with B = 1.25 − 2.5 µG and an angle of α = 15 − 45 • with respect to the upwind direction of the ISM flow generally provide the best fits to the data, but the sensitivity of the Lyα absorption to many model input parameters makes it difficult to fully characterize the region of parameter space allowed by the data. We also use the models to assess the degree to which heliospheric asymmetries induced by the ISM field should be apparent in Lyα absorption. An ISM field that is skewed with respect to the ISM flow vector results in substantial azimuthal asymmetries in both the hydrogen wall and heliosheath, but only the heliosheath asymmetries yield potentially detectable asymmetries in Lyα absorption; and then only in downwind directions, where comparison with the data is complicated by few actual absorption detections and an insufficient model grid extent.

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Cited by 5 publications

References 0 publications

Prompt $$\eta _c$$ meson production at the LHC in the NRQCD with $$k_T$$-factorization

Prompt $$\eta _c$$ meson production at the LHC in the NRQCD with $$k_T$$-factorization

Three-Dimensional Kinetic-MHD Model of the Global Heliosphere With the Heliopause-Surface Fitting

Dependence of Heliospheric Lyα Absorption on the Interstellar Magnetic Field

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