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3 results on '"cosmic radiation: TeV"'

1. Local fading accelerator and the origin of TeV cosmic ray electrons

Author

Jacco Vink, Stefano Gabici, S. Recchia, Felix Aharonian, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
electron: energy, lepton: energy, Inverse, Astrophysics, Electron, GeV, 01 natural sciences, cosmic radiation: TeV, Luminosity, Positron, Diffusion (business), attenuation, pulsar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, energy: high, cosmic radiation: spectrum, Computer Science::Computation and Language (Computational Linguistics and Natural Language and Speech Processing), shock waves, electron: spectrum, Supernova, positron, Production (computer science), Astrophysics - High Energy Astrophysical Phenomena, Particle physics, accelerator, Astrophysics::High Energy Astrophysical Phenomena, energy loss, Population, FOS: Physical sciences, Cosmic ray, cosmic radiation: diffusion, energy dependence, Pulsar, 0103 physical sciences, supernova, synchrotron, positron: acceleration, Fading, 010306 general physics, education, 010308 nuclear & particles physics, particle: energy, electron: cosmic radiation, acceleration, [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], injection, Compton scattering: inverse, 13. Climate action, Physics::Accelerator Physics, High Energy Physics::Experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Energy (signal processing), Astrophysics and astroparticle physics
Abstract

The cosmic ray electron spectrum exhibits a break at a particle energy of $\ensuremath{\sim}1\text{ }\text{ }\mathrm{TeV}$ and extends without any attenuation up to $\ensuremath{\sim}20\text{ }\text{ }\mathrm{TeV}$. Synchrotron and inverse Compton energy losses strongly constrain the time of emission of $\ensuremath{\sim}20\text{ }\text{ }\mathrm{TeV}$ electrons to $\ensuremath{\approx}2\ifmmode\times\else\texttimes\fi{}{10}^{4}\text{ }\text{ }\mathrm{yr}$ and the distance of the potential source(s) to $\ensuremath{\approx}100--500\text{ }\text{ }\mathrm{pc}$, depending on the cosmic ray diffusion coefficient. This suggests that maybe one nearby discrete source may explain the observed spectrum of high energy electrons. Given the strong energy dependence ($\ensuremath{\propto}1/E$) of the cooling time of TeV electrons, the spectral shape of the electron spectrum above the $\ensuremath{\sim}1\text{ }\text{ }\mathrm{TeV}$ break strongly depends on the history of injection of these electrons from the source. In this paper we show that a local, continuous (on timescales of $\ensuremath{\sim}{10}^{5}\text{ }\text{ }\mathrm{yr}$) but fading electron accelerator, with a characteristic decay time of $\ensuremath{\sim}{10}^{4}\text{ }\text{ }\mathrm{yr}$, can naturally account for the entire spectrum of cosmic ray electrons in the TeV domain. Although the standard ``nearby pulsar'' scenario naturally meets this time condition, it is (almost) excluded by recent measurements of the positron fraction, which above $\ensuremath{\sim}100\text{ }\text{ }\mathrm{GeV}$ saturates at a level well below 0.5 and drops above $\ensuremath{\sim}400--500\text{ }\text{ }\mathrm{GeV}$. The second potential source population, the supernova remnants, accelerate mostly electrons, rather than positrons. However, they hardly can provide an effective production of multi-TeV electrons via the standard diffusive shock acceleration scenario for $\ensuremath{\sim}{10}^{5}\text{ }\text{ }\mathrm{yr}$. A third possibility are stellar wind shocks, which however are likely to be continuous with nearly constant luminosity on timescales $\ensuremath{\gg}10\text{ }\text{ }\mathrm{kyr}$ and probably cannot match the time requirement of our potential source. Therefore, we face a real challenge in the identification of the origin of the source of multi-TeV electrons. Thus, the link of this source with known particle accelerators would require a dramatic revision of the standard paradigms of acceleration and escape in such objects.

Published
2019
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2. All-sky Measurement of the Anisotropy of Cosmic Rays at 10 TeV and Mapping of the Local Interstellar Magnetic Field

Author

HAWC Collaboration, Abeysekara, A. U., Brisbois, C., Becker, K. -H., Tjus, J. Becker, BenZvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Capistrán, T., Bohm, C., Börner, M., Bos, F., Böser, S., Botner, O., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Bretz, Hans-Peter, Carramiñana, A., Bron, S., Brostean-Kaiser, J., Burgman, A., Busse, R. S., Carver, T., Chen, C., Cheung, E., Chirkin, D., Clark, K., Classen, L., Casanova, S., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., Day, M., de André, J. P. A. M., De Clercq, C., Cotti, U., DeLaunay, J. J., Dembinski, H., Deoskar, K., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Díaz-Vélez, J. C., Cotzomi, J., Dujmovic, H., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Franckowiak, A., Friedman, E., Fritz, A., Gaisser, T. K., Gallagher, J., Ganster, E., Garrappa, S., De León, C., Gerhardt, L., Ghorbani, K., Giang, W., Glauch, T., Glüsenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Griffith, Z., Haack, C., De la Fuente, E., Hallgren, A., Halve, L., Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Dichiara, S., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Lankinen, Aapo, Huang, F., Huber, M., Hultqvist, K., Alfaro, R., DuVernois, M. A., Hünnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jacobi, Emanuel, Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Espinoza, C., Kalaczynski, P., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karle, A., Katz, U., Kauer, M., Keivani, A., Kelley, J. L., Fiorino, D. W., Kheirandish, A., Kim, J., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Köpke, L., Kopper, C., Fleischhack, H., Kopper, S., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Krückl, G., Kunwar, S., Kurahashi, N., Kyriacou, A., Labare, M., Fraija, N., Lanfranchi, J. L., Larson, M. J., Lauber, F., Leonard, K., Leuermann, M., Liu, Q. R., Lohfink, E., Mariscal, C. J. Lozano, Lu, L., Lünemann, J., Galván-Gámez, A., Luszczak, W., Madsen, J., Maggi, G., Mahn, K. B. M., Makino, Y., Mancina, S., Mariş, I. C., Maruyama, R., Mase, K., Maunu, R., García-González, J. A., Meagher, K., Medici, M., Medina, A., Meier, M., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Momenté, G., González, M. M., Montaruli, T., Moore, R. W., Moulai, M., Nagai, R., Nahnhauer, R., Nakarmi, P., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Goodman, J. A., Nygren, D. R., Pollmann, A. Obertacke, Olivas, A., O'Murchadha, A., O'Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Heros, C. Pérez de los, Hampel-Arias, Z., Pieloth, D., Pinat, E., Pizzuto, A., Plum, M., Price, P. B., Przybylski, G. T., Raab, C., Raissi, A., Rameez, M., Rauch, L., Alvarez, C., Harding, J. P., Rawlins, K., Rea, I. C., Reimann, R., Relethford, B., Renzi, G., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Hernandez, S., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Safa, I., Herrera, S. E. Sanchez, Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Hona, B., Satalecka, K., Schaufel, M., Schlunder, P., Schmidt, T., Schneider, A., Schneider, J., Schöneberg, S., Schumacher, L., Sclafani, S., Hueyotl-Zahuantitla, F., Seckel, D., Seunarine, S., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Iriarte, A., Stasik, Alexander, Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stößl, A., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Jardin-Blicq, A., Sutherland, M., Taboada, I., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Tobin, M. N., Tönnis, C., Toscano, S., Tosi, D., Joshi, V., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Ty, B., Unger, E., Elorrieta, M. A. Unland, Usner, Marcel, Vandenbroucke, J., Lara, A., Van Driessche, W., van Eijk, D., van Eijndhoven, N., Vanheule, S., van Santen, J., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandkowsky, N., Vargas, H. León, Wandler, F. D., Watson, T. B., Weaver, C., Weiss, M. J., Weldert, J., Wendt, C., Werthebach, J., Westerhoff, S., Whelan, B. J., Whitehorn, N., Luis-Raya, G., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, J., Wood, T. R., Woolsey, E., Woschnagg, K., Álvarez, J. D., Malone, K., Wrede, G., Xu, D. L., Xu, X. W., Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Yuan, T., IceCube Collaboration, Marinelli, S. S., Martínez-Castro, J., Martinez, O., Matthews, J. A., Miranda-Romagnoli, P., Moreno, E., Mostafá, M., Nellen, L., Newbold, M., Arceo, R., Nisa, M. U., Noriega-Papaqui, R., Pérez-Pérez, E. G., Pretz, J., Ren, Z., Rho, C. D., Rivière, C., Rosa-González, D., Rosenberg, M., Salazar, H., Arteaga-Velázquez, J. C., Greus, F. Salesa, Sandoval, A., Schneider, M., Schoorlemmer, H., Sinnis, G., Smith, A. J., Surajbali, P., Tollefson, K., Torres, I., Rojas, D. Avila, Villaseño, L., Weisgarber, T., Zepeda, A., Zhou, H., Techn. Koordinator:, J. Spengler, Aartsen, M. G., Ackermann, M., Adams, J., Belmont-Moreno, E., Aguilar, J. A., Ahlers, M., Ahrens, M., Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Argüelles, C., Auffenberg, J., BenZvi, S. Y., Axani, S., Backes, P., Bagherpour, H., Bai, X., Barbano, A., Barron, J. P., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Physics, and Elementary Particle Physics

Subjects
010504 meteorology & atmospheric sciences, TeV [cosmic radiation], magnetic field, Astrophysics, anisotropy [cosmic radiation], 01 natural sciences, cosmic radiation: TeV, IceCube, 3-DIMENSIONAL FEATURES, propagation, Anisotropy, 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, angular dependence [power spectrum], Astrophysics::Instrumentation and Methods for Astrophysics, ENERGY-SPECTRUM, Magnetic field, astroparticle physics, cosmic rays, ISM: magnetic fields, observatory, power spectrum: angular dependence, Physique des particules élémentaires, Astrophysics - High Energy Astrophysical Phenomena, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, LARGE-SCALE ANISOTROPY, Astrophysics::Cosmology and Extragalactic Astrophysics, energy [particle], cosmic radiation: anisotropy, 0103 physical sciences, ARRIVAL DIRECTIONS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, INTENSITY, particle: energy, magnetic fields [ISM], Spectral density, Astronomy and Astrophysics, OUTER HELIOSPHERE, Interstellar medium, Dipole, Physics and Astronomy, Space and Planetary Science, Sky, ROTATION, ddc:520, HAWC, Energy (signal processing), dipole
Abstract

We present the first full-sky analysis of the cosmic ray arrival direction distribution with data collected by the High-Altitude Water Cherenkov and IceCube observatories in the northern and southern hemispheres at the same median primary particle energy of 10 TeV. The combined sky map and angular power spectrum largely eliminate biases that result from partial sky coverage and present a key to probe into the propagation properties of TeV cosmic rays through our local interstellar medium and the interaction between the interstellar and heliospheric magnetic fields. From the map, we determine the horizontal dipole components of the anisotropy δ 0h = 9.16 ×10 -4 and δ 6h = 7.25 ×10 -4 (±0.04 × 10 -4 ). In addition, we infer the direction (229.°2 ± 3.°5 R.A. 11.°4 ± 3.°0 decl.) of the interstellar magnetic field from the boundary between large-scale excess and deficit regions from which we estimate the missing corresponding vertical dipole component of the large-scale anisotropy to be δN ∼ -3.97 +1.0 -2.0 × 10 -4 ., 0, SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2019
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3. The cosmic-ray content of the Orion-Eridanus superbubble

Author

I. A. Grenier, Reinhard Schlickeiser, T. Tolksdorf, J. M. Casandjian, T. Joubaud, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut für Theoretische Physik IV [Bochum] (ITP4), Ruhr-Universität Bochum [Bochum], ANR-15-CE31-0019,CRiBs,Rayons Cosmiques dans les super Bulles(2015), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, halo, FOS: Physical sciences, magnetic field, Cosmic ray, Superbubble, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, cosmic radiation: interaction, cosmic radiation: TeV, 01 natural sciences, GLAST, Galactic halo, cosmic rays, gas, supernova, 0103 physical sciences, cloud, Eridanus, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, cosmic radiation: production, acceleration of particles, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, polarization, cosmic radiation: spectrum, particle: energy, Computer Science::Information Retrieval, turbulence, Astronomy and Astrophysics, Galactic plane, Orion–Eridanus Superbubble, solar, Galaxy: halo, star: massive, Supernova, gamma ray, 13. Climate action, Space and Planetary Science, spectral, galaxy, Halo, Astrophysics - High Energy Astrophysical Phenomena, ISM: bubbles, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic radiation: flux, local insterstellar matter
Abstract

The nearby Orion-Eridanus superbubble, which was blown by multiple supernovae several Myr ago, has likely produced cosmic rays. Its turbulent medium, still energised by massive stars, can impact cosmic-ray transport locally. The gamma rays produced in cosmic-ray interactions with interstellar gas were used to compare the GeV to TeV cosmic-ray spectrum in the superbubble and in other regions near the Sun. We used ten years of Fermi-LAT data in the 0.25-63 GeV energy range to study the closer (Eridanus) end of the superbubble. We modelled the spatial and spectral distributions of the gamma rays produced in the different gas phases of the clouds found in this direction. We found that the gamma-ray emissivity spectrum of the gas along the outer rim and in a shell inside the superbubble is consistent with the average spectrum measured in the solar neighbourhood. This result calls for a detailed assessment of the recent supernova rate and census of massive stellar winds in the superbubble in order to estimate the epoch and rate of cosmic-ray production and to constrain the transport conditions that can lead to such homogeneity and little re-acceleration. We also found significant evidence that a diffuse cloud lying outside the superbubble, at a height of 200-250 pc below the Galactic plane, is pervaded by a 34\% lower cosmic-ray flux, but with the same particle energy distribution as the local one. Super-GeV cosmic rays should freely cross such a diffuse atomic cloud without significant loss or spectral distorsion. We tentatively propose that the cosmic-ray loss relates to the orientation of the magnetic field lines threading the cirrus, which point towards the halo according to the dust polarisation data. We gathered past and present emissivity measurements near the Sun to show how the local cosmic-ray flux decreases with Galactic height and to compare this trend with model predictions., Comment: 20 pages, 17 figures, accepted for publication in Astronomy & Astrophysics

Published
2020
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