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Готові списки джерел за темами / Stellar cosmic rays / Статті в журналах

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Статті в журналах з теми "Stellar cosmic rays"

Автор: Grafiati

Опубліковано: 3 червня 2025

Оновлено: 31 липня 2025

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1

Rodgers-Lee, D., A. M. Taylor, A. A. Vidotto, and T. P. Downes. "Stellar versus Galactic: the intensity of cosmic rays at the evolving Earth and young exoplanets around Sun-like stars." Monthly Notices of the Royal Astronomical Society 504, no. 1 (2021): 1519–30. http://dx.doi.org/10.1093/mnras/stab935.

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ABSTRACT Energetic particles, such as stellar cosmic rays, produced at a heightened rate by active stars (like the young Sun) may have been important for the origin of life on Earth and other exoplanets. Here, we compare, as a function of stellar rotation rate (Ω), contributions from two distinct populations of energetic particles: stellar cosmic rays accelerated by impulsive flare events and Galactic cosmic rays. We use a 1.5D stellar wind model combined with a spatially 1D cosmic ray transport model. We formulate the evolution of the stellar cosmic ray spectrum as a function of stellar rotat

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2

Mesquita, A. L., D. Rodgers-Lee, and A. A. Vidotto. "The Earth-like Galactic cosmic ray intensity in the habitable zone of the M dwarf GJ 436." Monthly Notices of the Royal Astronomical Society 505, no. 2 (2021): 1817–26. http://dx.doi.org/10.1093/mnras/stab1483.

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ABSTRACT Galactic cosmic rays are energetic particles important in the context of life. Many works have investigated the propagation of Galactic cosmic rays through the Sun’s heliosphere. However, the cosmic ray fluxes in M dwarf systems are still poorly known. Studying the propagation of Galactic cosmic rays through the astrospheres of M dwarfs is important to understand the effect on their orbiting planets. Here, we focus on the planetary system GJ 436. We perform simulations using a combined 1D cosmic ray transport model and 1D Alfvén-wave-driven stellar wind model. We use two stellar wind

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3

Biermann, Peter L. "Cosmic rays, stellar evolution and supernova physics." New Astronomy Reviews 48, no. 1-4 (2004): 41–46. http://dx.doi.org/10.1016/j.newar.2003.11.006.

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4

Rodgers-Lee, D., A. A. Vidotto, and A. L. Mesquita. "Charting nearby stellar systems: the intensity of Galactic cosmic rays for a sample of solar-type stars." Monthly Notices of the Royal Astronomical Society 508, no. 4 (2021): 4696–704. http://dx.doi.org/10.1093/mnras/stab2788.

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ABSTRACT Cosmic rays can penetrate planetary atmospheres driving the formation of prebiotic molecules, which are important for the origin of life. We calculate the Galactic cosmic ray fluxes in the habitable zone (HZ) of five nearby, well-studied solar-type stars and at the orbits of two known exoplanets. We model the propagation of Galactic cosmic rays through the stellar winds using a combined 1.5D stellar wind and 1D cosmic ray transport model. We find that the HZ of 61 Cyg A has comparable Galactic cosmic ray fluxes to present-day Earth values. For the other four systems (ϵ Eri, ϵ Ind, ξ B

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5

de Menezes, Raniere, Elena Orlando, Mattia Di Mauro, and Andrew Strong. "A study of superluminous stars with the Fermi-Large Area Telescope." Monthly Notices of the Royal Astronomical Society 507, no. 1 (2021): 680–86. http://dx.doi.org/10.1093/mnras/stab2150.

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ABSTRACT The γ-ray emission from stars is induced by the interaction of cosmic rays with stellar atmospheres and photon fields. This emission is expected to come in two components: a stellar disc emission, where γ-rays are mainly produced in atmospheric showers generated by hadronic cosmic rays, and an extended halo emission, where the high density of soft photons in the surroundings of stars create a suitable environment for γ-ray production via inverse Compton (IC) scattering by cosmic ray electrons. Besides the Sun, no other disc or halo from single stars has ever been detected in γ-rays. H

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6

Mesquita, A. L., D. Rodgers-Lee, A. A. Vidotto, D. Atri, and B. E. Wood. "Galactic cosmic ray propagation through M dwarf planetary systems." Monthly Notices of the Royal Astronomical Society 509, no. 2 (2021): 2091–101. http://dx.doi.org/10.1093/mnras/stab3131.

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ABSTRACT Quantifying the flux of cosmic rays reaching exoplanets around M dwarfs is essential to understand their possible effects on exoplanet habitability. Here, we investigate the propagation of Galactic cosmic rays as they travel through the stellar winds (astrospheres) of five nearby M dwarfs, namely: GJ 15A, GJ 273, GJ 338B, GJ 411, and GJ 887. Our selected stars each have one or two detected exoplanets and they all have wind mass-loss rates constrained by Lyman α observations. Our simulations use a combined 1D magnetohydrodynamic (MHD) Alfvén-wave-driven stellar wind model and 1D cosmic

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7

Joubaud, T., I. A. Grenier, J. M. Casandjian, T. Tolksdorf, and R. Schlickeiser. "The cosmic-ray content of the Orion-Eridanus superbubble." Astronomy & Astrophysics 635 (March 2020): A96. http://dx.doi.org/10.1051/0004-6361/201937205.

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Aims. The nearby Orion-Eridanus superbubble, which was blown by multiple supernovae several million years ago, has likely produced cosmic rays. Its turbulent medium is still energised by massive stellar winds and it can impact cosmic-ray transport locally. The γ radiation produced in interactions between cosmic rays and interstellar gas can be used to compare the cosmic-ray spectrum in the superbubble and in other regions near the Sun. It can reveal spectral changes induced in GeV to TeV cosmic rays by the past and present stellar activity in the superbubble. Methods. We used ten years of data

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8

Tanaka, S., S. Kitamoto, T. Suzuki, K. Torii, M. F. Corcoran, and W. Waldron. "Chemical Abundances of Early Type Stars." Symposium - International Astronomical Union 188 (1998): 224–25. http://dx.doi.org/10.1017/s007418090011486x.

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X-rays from early-type stars are emitted by the corona or the stellar wind. The materials in the surface layer of early-type stars are not contaminated by nuclear reactions in the stellar inside. Therefore, abundance study of the early-type stars provides us an information of the abundances of the original gas. However, the X-ray observations indicate low-metallicity, which is about 0.3 times of cosmic abundances. This fact raises the problem on the cosmic abundances.

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9

Tagawa, Hiromichi, Shigeo S. Kimura, and Zoltán Haiman. "High-energy Electromagnetic, Neutrino, and Cosmic-Ray Emission by Stellar-mass Black Holes in Disks of Active Galactic Nuclei." Astrophysical Journal 955, no. 1 (2023): 23. http://dx.doi.org/10.3847/1538-4357/ace71d.

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Abstract Some Seyfert galaxies are detected in high-energy gamma rays, but the mechanism and site of gamma-ray emission are unknown. Also, the origins of the cosmic high-energy neutrino and MeV gamma-ray backgrounds have been veiled in mystery since their discoveries. We propose emission from stellar-mass BHs (sBHs) embedded in disks of active galactic nuclei as their possible sources. These sBHs are predicted to launch jets due to the Blandford–Znajek mechanism, which can produce intense electromagnetic, neutrino, and cosmic-ray emissions. We investigate whether these emissions can be the sou

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10

Mirabel, I. F. "Microquasars as Sources of High Energy Phenomena." Symposium - International Astronomical Union 214 (2003): 201–10. http://dx.doi.org/10.1017/s0074180900194409.

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Relativistic outflows are a common phenomenon in accreting black holes. Despite the enormous differences in scale, accreting stellar-mass black holes (X-ray binaries, collapsars) and super-massive black holes produce jets with analogous physical properties. Here I review microquasars as sources of relativistic jets, gamma-rays, cosmic rays, and high energy neutrinos.

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11

Lee, T. "Proto-Stellar Cosmic Rays and Extinct Radioactivities in Meteorites." Mineralogical Magazine 62A, no. 2 (1998): 872. http://dx.doi.org/10.1180/minmag.1998.62a.2.125.

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12

Westphal, Andrew J., P. Buford Price, Benjamin A. Weaver, and Vladimir G. Afanasiev. "Evidence against stellar chromospheric origin of Galactic cosmic rays." Nature 396, no. 6706 (1998): 50–52. http://dx.doi.org/10.1038/23887.

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13

Ko, Chung-Ming, and Min-Hsu Chu. "Self-similar solutions to stellar winds with cosmic rays." Advances in Space Research 35, no. 12 (2005): 2115–18. http://dx.doi.org/10.1016/j.asr.2005.03.002.

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14

Sinitsyna, V. G., V. Y. Sinitsyna, and Yu I. Stozhkov. "Galactic Cosmic Rays: The first detection of TeV gamma-rays from Red Dwarfs." EPJ Web of Conferences 208 (2019): 14007. http://dx.doi.org/10.1051/epjconf/201920814007.

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The present point of view on the sources of cosmic rays in Galaxy considers explosions of supernovae as sources of these particles up to energies of 1017 eV. However, the experimental data obtained with Pamela, Fermi, AMS-02 spectrometers requires the existence of nearby sources of cosmic rays at distances less then 1 kpc from the solar system. These sources could explain such experimental data as the growth of the ratio of galactic positrons to electrons with increasing energy, the complex dependence of the exponent of the proton and alpha spectra from the energy of these particles, the appea

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15

Rodgers-Lee, D., A. A. Vidotto, A. M. Taylor, P. B. Rimmer, and T. P. Downes. "The Galactic cosmic ray intensity at the evolving Earth and young exoplanets." Monthly Notices of the Royal Astronomical Society 499, no. 2 (2020): 2124–37. http://dx.doi.org/10.1093/mnras/staa2737.

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ABSTRACT Cosmic rays may have contributed to the start of life on the Earth. Here, we investigate the evolution of the Galactic cosmic ray spectrum at the Earth from ages t = 0.6−6.0 Gyr. We use a 1D cosmic ray transport model and a 1.5D stellar wind model to derive the evolving wind properties of a solar-type star. At $t=1\,$ Gyr, approximately when life is thought to have begun on the Earth, we find that the intensity of ∼GeV Galactic cosmic rays would have been ∼10 times smaller than the present-day value. At lower kinetic energies, Galactic cosmic ray modulation would have been even more s

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16

O’Donoghue, Ross, Serena Viti, Marco Padovani, and Tomas James. "The Effects of Cosmic Rays on the Chemistry of Dense Cores." Astrophysical Journal 934, no. 1 (2022): 63. http://dx.doi.org/10.3847/1538-4357/ac7963.

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Abstract Cosmic rays are crucial to the chemistry of molecular clouds and their evolution. They provide essential ionizations, dissociations, heating, and energy to the cold, dense cores. As cosmic rays pierce through clouds they are attenuated and lose energy, which leads to a dependency on the column density of a system. The detailed effects these particles have on the central regions still need to be fully understood. Here, we revisit how cosmic rays are treated in the UCLCHEM chemical modeling code by including both ionization rate and H2 dissociation rate dependencies alongside the produc

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17

Farber, Ryan J., Mateusz Ruszkowski, Stephanie Tonnesen, and Francisco Holguin. "Stress-testing cosmic ray physics: the impact of cosmic rays on the surviving disc of ram-pressure-stripped galaxies." Monthly Notices of the Royal Astronomical Society 512, no. 4 (2022): 5927–41. http://dx.doi.org/10.1093/mnras/stac794.

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ABSTRACT Cluster spiral galaxies suffer catastrophic losses of the cool, neutral gas component of their interstellar medium due to ram pressure stripping, contributing to the observed quenching of star formation in the disc compared to galaxies in lower density environments. However, the short-term effects of ram pressure on the star formation rate and active galactic nucleus (AGN) activity of galaxies undergoing stripping remain unclear. Numerical studies have recently demonstrated cosmic rays can dramatically influence galaxy evolution for isolated galaxies, yet their influence on ram pressu

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18

Brandt, S., N. Lund, and A. R. Rao. "Solar and Stellar Flare Observations using Watch." International Astronomical Union Colloquium 104, no. 2 (1989): 33–36. http://dx.doi.org/10.1017/s0252921100153746.

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AbstractThe Danish experiment WATCH (Wide Angle Telescope for Cosmic Hard X-rays) is to be flown on board the Soviet satellite GRANAT in middle of 1989. The performence characteristics of the WATCH instrument is described. It is estimated that WATCH can detect about 100 solar hard X-ray bursts per day. WATCH can also detect about 40 energetic stellar soft X-ray flares, similar to the fast transient X-ray emissions detected by the Ariel V satellite.

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19

Marafico, Sullivan, Jonathan Biteau, Antonio Condorelli, Olivier Deligny, and Quentin Luce. "Observational constraints on accelerators of ultra-high energy cosmic rays." Journal of Physics: Conference Series 2429, no. 1 (2023): 012012. http://dx.doi.org/10.1088/1742-6596/2429/1/012012.

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Abstract We explore two generic hypotheses for tracing the sources of ultra-high energy cosmic rays (UHECRs) in the Universe: star formation rate density or stellar mass density. For each scenario, we infer a set of constraints for the emission mechanisms in the accelerators, for their energetics and for the abundances of elements at escape from their environments. From these constraints, we generate sky maps above 40 EeV expected from a catalog that comprises 410,761 galaxies out to 350 Mpc and provides a near-infrared flux-limited sample to map both stellar mass and star formation rate over

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20

Olmi, Barbara, Giovanni Morlino, and Niccolò Bucciantini. "A broadband excursus through stellar afterlife." Il Colle di Galileo 14, no. 1 (2025): 83–85. https://doi.org/10.36253/cdg-16138.

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The workshop drew experts from the Supernova Remnants, Pulsars and Pulsar Wind Nebulae communities, both from a multi-wavelengths observational point of view and a theoretical perspective. Recent developments in these fields were discussed, with broader coverage of the related physical processes (such as acceleration and propagation of particles, relevance of the sources for Galactic Cosmic Rays). Particular attention was also devoted to statistical methods in astrophysics. The workshop also provided an opportunity to celebrate the career of Rino Bandiera who successfully dedicated most of his

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21

C. Beers, Timothy, Takeru K. Suzuki, and Yuzuru Yoshii. "The Light Elements Be and B as Stellar Chronometers in the Early Galaxy." Symposium - International Astronomical Union 198 (2000): 425–31. http://dx.doi.org/10.1017/s0074180900167002.

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Recent detailed simulations of Galactic Chemical Evolution have shown that the heavy elements, in particular [Fe/H], are expected to exhibit a weak, or absent, correlation with stellar ages in the early Galaxy due to the lack of efficient mixing of interstellar material enriched by individual Type II supernovae. A promising alternative ‘chronometer’ of stellar ages is suggested, based on the expectation that the light elements Be and B are formed primarily as spallation products of Galactic Cosmic Rays.

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22

Nozzoli, Francesco, and Cinzia Cernetti. "Beryllium Radioactive Isotopes as a Probe to Measure the Residence Time of Cosmic Rays in the Galaxy and Halo Thickness: A “Data-Driven” Approach." Universe 7, no. 6 (2021): 183. http://dx.doi.org/10.3390/universe7060183.

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Cosmic rays are a powerful tool for the investigation of the structure of the magnetic fields in the Galactic halo and the properties of the inter-stellar medium. Two parameters of the cosmic ray propagation models, the Galactic halo (half) thickness, H, and the diffusion coefficient, D, are loosely constrained by current cosmic ray flux measurements; in particular, a large degeneracy exists, with only H/D being well measured. The 10Be/9Be isotopic flux ratio (thanks to the 2 My lifetime of 10Be) can be used as a radioactive clock providing the measurement of cosmic ray residence time in a gal

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23

Nickeler, D. H., T. Wiegelmann, M. Karlický, and M. Kraus. "MHD flows at astropauses and in astrotails." ASTRA Proceedings 1 (September 5, 2014): 51–60. http://dx.doi.org/10.5194/ap-1-51-2014.

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Abstract. The geometrical shapes and the physical properties of stellar wind – interstellar medium interaction regions form an important stage for studying stellar winds and their embedded magnetic fields as well as cosmic ray modulation. Our goal is to provide a proper representation and classification of counter-flow configurations and counter-flow interfaces in the frame of fluid theory. In addition we calculate flows and large-scale electromagnetic fields based on which the large-scale dynamics and its role as possible background for particle acceleration, e.g., in the form of anomalous co

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24

Meyer, J. P. "Solar-stellar outer atmospheres and energetic particles, and galactic cosmic rays." Astrophysical Journal Supplement Series 57 (January 1985): 173. http://dx.doi.org/10.1086/191001.

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25

Cleeves, L. Ilsedore, Fred C. Adams, and Edwin A. Bergin. "EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS." Astrophysical Journal 772, no. 1 (2013): 5. http://dx.doi.org/10.1088/0004-637x/772/1/5.

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26

Gurzadyan, G. A. "The activity of stellar aggregates and the origin of cosmic rays." Astrophysics and Space Science 113, no. 2 (1985): 213–31. http://dx.doi.org/10.1007/bf00650958.

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27

Diehl, Roland, and Maria Lugaro. "Astronomy with Radioactivities." Publications of the Astronomical Society of Australia 29, no. 2 (2012): 87–89. http://dx.doi.org/10.1071/as12010.

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Cosmic radioactivity represents a cross-disciplinary theme and an interesting alternate viewpoint on cosmic nuclear astrophysics. Radioactive isotopes and their decay provide unique messages from sites of cosmic nucleosynthesis, as the decay is mediated by weak interaction physics and independent of environmental conditions. The radioactive clock of various isotopes traces stellar mixing processes and the process of solidification of bodies when the solar system was formed. Isotopic abundances directly reflect the conditions of their formation in the nucleosynthesis site, which is unobservable

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28

Duarte, Eduardo Seperuelo, Alicja Domaracka, Philippe Boduch, et al. "Heavy ion irradiation of astrophysical ice analogs." Proceedings of the International Astronomical Union 5, S263 (2009): 29–32. http://dx.doi.org/10.1017/s1743921310001444.

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AbstractIcy grain mantles consist of small molecules containing hydrogen, carbon, oxygen and nitrogen atoms (e.g. H2O, CO, CO2, NH3). Such ices, present in different astrophysical environments (giant planets satellites, comets, dense clouds, and protoplanetary disks), are subjected to irradiation of different energetic particles: UV radiation, ion bombardment (solar and stellar wind as well as galactic cosmic rays), and secondary electrons due to cosmic ray ionization of H2. The interaction of these particles with astrophysical ice analogs has been the object of research over the last decades.

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29

Mirabel, I. F. "Black hole high mass X-ray binary microquasars at cosmic dawn." Proceedings of the International Astronomical Union 14, S346 (2018): 365–79. http://dx.doi.org/10.1017/s1743921319002084.

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AbstractTheoretical models and observations suggest that primordial Stellar Black Holes (Pop-III-BHs) were prolifically formed in HMXBs, which are powerful relativistic jet sources of synchrotron radiation called Microquasars (MQs).Large populations of BH-HMXB-MQs at cosmic dawn produce a smooth synchrotron cosmic radio background (CRB) that could account for the excess amplitude of atomic hydrogen absorption at z∼17, recently reported by EDGES.BH-HMXB-MQs at cosmic dawn precede supernovae, neutron stars and dust. BH-HMXB-MQs promptly inject into the IGM hard X-rays and relativistic jets, whic

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30

Washinoue, Haruka, Shinsuke Takasao, and Kenji Furuya. "Effect of Time-varying X-Ray Emission from Stellar Flares on the Ionization of Protoplanetary Disks." Astrophysical Journal 976, no. 1 (2024): 25. http://dx.doi.org/10.3847/1538-4357/ad7fdf.

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Abstract X-rays have significant impacts on cold, weakly ionized protoplanetary disks by increasing the ionization rate and driving chemical reactions. Stellar flares are explosions that emit intense X-rays and are the unique source of hard X-rays with an energy of ≳10 keV in the protoplanetary disk systems. Hard X-rays should be carefully taken into account in models as they can reach the disk midplane as a result of scattering in the disk atmospheres. However, previous models are insufficient to predict the hard X-ray spectra because of simplifications in flare models. We develop a model of

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31

Vidotto, A. A. "Incorporating magnetic field observations in wind models of low-mass stars." ASTRA Proceedings 1 (June 6, 2014): 19–22. http://dx.doi.org/10.5194/ap-1-19-2014.

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Abstract. Stellar winds of cool, main-sequence stars are very tenuous and difficult to observe. Despite carrying away only a small amount of the stellar mass, they are important for regulating the rotation of the star and, consequently, its activity and magnetism. As it permeates the interplanetary space, the stellar wind interacts with any exoplanet encountered on its way, until it reaches the interstellar medium (ISM). These interactions can result in complex physical processes that depend on the characteristics of the wind. To better constrain the wind characteristics, more realistic wind m

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32

Su, Kung-Yi, Philip F. Hopkins, Christopher C. Hayward, et al. "The failure of stellar feedback, magnetic fields, conduction, and morphological quenching in maintaining red galaxies." Monthly Notices of the Royal Astronomical Society 487, no. 3 (2019): 4393–408. http://dx.doi.org/10.1093/mnras/stz1494.

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ABSTRACT The quenching ‘maintenance’ and related ‘cooling flow’ problems are important in galaxies from Milky Way mass through clusters. We investigate this in haloes with masses ∼$10^{12}\!-\!10^{14}\, {\rm M}_{\odot }$, using non-cosmological high-resolution hydrodynamic simulations with the FIRE-2 (Feedback In Realistic Environments) stellar feedback model. We specifically focus on physics present without AGN, and show that various proposed ‘non-AGN’ solution mechanisms in the literature, including Type Ia supernovae, shocked AGB winds, other forms of stellar feedback (e.g. cosmic rays), ma

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33

Fatuzzo, Marco, Fred C. Adams, Adina D. Feinstein, and Darryl Z. Seligman. "Avalanches and the Distribution of Reconnection Events in Magnetized Circumstellar Disks." Astrophysical Journal 954, no. 1 (2023): 15. http://dx.doi.org/10.3847/1538-4357/ace909.

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Abstract Cosmic rays produced by young stellar objects can potentially alter the ionization structure, heating budget, chemical composition, and accretion activity in circumstellar disks. The inner edges of these disks are truncated by strong magnetic fields, which can reconnect and produce flaring activity that accelerates cosmic radiation. The resulting cosmic rays can provide a source of ionization and produce spallation reactions that alter the composition of planetesimals. These reconnection and particle acceleration processes are analogous to the physical processes that produce flaring i

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34

Heesen, Volker, Aritra Basu, Elias Brinks, et al. "Stellar feedback in dwarf irregular galaxies with radio continuum observations." Proceedings of the International Astronomical Union 14, S344 (2018): 255–58. http://dx.doi.org/10.1017/s1743921318006841.

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AbstractLow-mass dwarf irregular galaxies are subject to outflows, in which cosmic rays may play a very important role; they can be traced via their electron component, the cosmic ray electrons (CRe), in the radio continuum as non-thermal synchrotron emission. With the advent of sensitive low-frequency observations, such as with the Low-Frequency Array (LOFAR), we can trace CRe far away from star formation sites. Together with GHz-observations, such as with the Very Large Array (VLA), we can study spatially resolved radio continuum spectra at matched angular resolution and sensitivity. Here, w

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35

Rathjen, Tim-Eric, Thorsten Naab, Philipp Girichidis, et al. "SILCC VI – Multiphase ISM structure, stellar clustering, and outflows with supernovae, stellar winds, ionizing radiation, and cosmic rays." Monthly Notices of the Royal Astronomical Society 504, no. 1 (2021): 1039–61. http://dx.doi.org/10.1093/mnras/stab900.

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ABSTRACT We present simulations of the multiphase interstellar medium (ISM) at solar neighbourhood conditions including thermal and non-thermal ISM processes, star cluster formation, and feedback from massive stars: stellar winds, hydrogen ionizing radiation computed with the novel treeray radiative transfer method, supernovae (SN), and the injection of cosmic rays (CR). N-body dynamics is computed with a 4th-order Hermite integrator. We systematically investigate the impact of stellar feedback on the self-gravitating ISM with magnetic fields, CR advection and diffusion, and non-equilibrium ch

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36

Kalinin, M. S., and M. B. Krainev. "The Galactic Cosmic Rays and the Interaction Between Solar and Stellar Winds." Advances in Space Research 13, no. 6 (1993): 295. http://dx.doi.org/10.1016/0273-1177(93)90428-e.

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37

Güdel, Manuel. "Observational constraints for solar-type Stellar winds." Proceedings of the International Astronomical Union 15, S354 (2019): 313–32. http://dx.doi.org/10.1017/s1743921320001441.

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AbstractIonized winds from late-type main-sequence stars are important for stellar spin-down and therefore the evolution of stellar activity; winds blow an “astrosphere” into the interstellar medium that absorbs a large part of galactic cosmic rays; and the winds play a key role in shaping planetary environments, in particular their upper atmospheres. These issues have been well studied for the solar wind but little is known about winds escaping from other solar-type stars. Several methods have been devised to either detect winds directly or to infer the presence of such winds from features th

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38

Lacki, Brian C. "Galactic traversability: a new concept for extragalactic SETI." International Journal of Astrobiology 20, no. 5 (2021): 359–76. http://dx.doi.org/10.1017/s1473550421000252.

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AbstractInterstellar travel in the Milky Way is commonly thought to be a long and dangerous enterprise, but are all galaxies so hazardous? I introduce the concept of galactic traversability to address this question. Stellar populations are one factor in traversability, with higher stellar densities and velocity dispersions aiding rapid spread across a galaxy. The interstellar medium (ISM) is another factor, as gas, dust grains and cosmic rays all pose hazards to starfarers. I review the current understanding of these components in different types of galaxies, and conclude that red quiescent ga

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39

MIROSHNICHENKO, L. I., and J. A. PEREZ-PERAZA. "ASTROPHYSICAL ASPECTS IN THE STUDIES OF SOLAR COSMIC RAYS." International Journal of Modern Physics A 23, no. 01 (2008): 1–141. http://dx.doi.org/10.1142/s0217751x08037312.

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This review paper comprises main concepts, available observational data and recent theoretical results related to astrophysical aspects of particle acceleration at/near the Sun and extreme capacities of the solar accelerator(s). We summarize underground and ground-based observations of solar cosmic rays (SCR) accumulated since 1942, direct spacecraft measurements of solar energetic particles (SEP) near the Earth's orbit, indirect information on the SCR variations in the past, and other relevant astrophysical, solar and geophysical data. The list of the problems under discussion includes: upper

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40

Ochmas, Nastaran. "Dust and Ice in the Interstellar Medium." Journal for Research in Applied Sciences and Biotechnology 3, no. 1 (2024): 358–62. http://dx.doi.org/10.55544/jrasb.3.1.54.

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In this paper, we present an introduction to bare dust particles and grains covered by ice sheets in diffuse and dense interstellar clouds. It follows the life cycle of dust from its formation in stellar environments to its incorporation into the body of the Solar system. Dust particles play an important role in the physics and chemistry of many space environments. Regarding dust composition, two different populations are generally observed: silicate and carbonaceous dust. Energetic processing of ice layers with UV rays, X – rays or cosmic rays, after which the heat leads to the formation of c

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41

Quataert, Eliot, Todd A. Thompson, and Yan-Fei Jiang (姜燕飞). "The physics of galactic winds driven by cosmic rays I: Diffusion." Monthly Notices of the Royal Astronomical Society 510, no. 1 (2021): 1184–203. http://dx.doi.org/10.1093/mnras/stab3273.

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ABSTRACT The physics of Cosmic ray (CR) transport remains a key uncertainty in assessing whether CRs can produce galaxy-scale outflows consistent with observations. In this paper, we elucidate the physics of CR-driven galactic winds for CR transport dominated by diffusion. A companion paper considers CR streaming. We use analytic estimates validated by time-dependent spherically symmetric simulations to derive expressions for the mass-loss rate, momentum flux, and speed of CR-driven galactic winds, suitable for cosmological-scale or semi-analytic models of galaxy formation. For CR diffusion co

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42

Ávila, Patricio Javier, Tommaso Grassi, Stefano Bovino, et al. "Presence of water on exomoons orbiting free-floating planets: a case study." International Journal of Astrobiology 20, no. 4 (2021): 300–311. http://dx.doi.org/10.1017/s1473550421000173.

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AbstractA free-floating planet (FFP) is a planetary-mass object that orbits around a non-stellar massive object (e.g. a brown dwarf) or around the Galactic Centre. The presence of exomoons orbiting FFPs has been theoretically predicted by several models. Under specific conditions, these moons are able to retain an atmosphere capable of ensuring the long-term thermal stability of liquid water on their surface. We model this environment with a one-dimensional radiative-convective code coupled to a gas-phase chemical network including cosmic rays and ion-neutral reactions. We find that, under spe

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43

Sorli, Amrit Srecko. "Black Holes are Rejuvenating Systems of the Universe." JOURNAL OF ADVANCES IN PHYSICS 17 (January 21, 2020): 23–31. http://dx.doi.org/10.24297/jap.v17i.8620.

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Recent research on superfluid quantum vacuum as the physical origin of universal space has opened new perspectives in astronomy and cosmology. Every stellar object is in the active relation with space and its density diminishes according to the mass-energy equivalence principle. As per Newton’s Shell Theorem, vacuum density is minimum at the surface of the stellar objects and in their centre. The density of space on the surface of the Black holes and in their centre is so low that atoms become unstable. Therefore, they disintegrate back into the elementary particles and cosmic rays. By transfo

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44

Tabataba-Vakili, F., J. L. Grenfell, J. M. Grießmeier, and H. Rauer. "Atmospheric effects of stellar cosmic rays on Earth-like exoplanets orbiting M-dwarfs." Astronomy & Astrophysics 585 (December 23, 2015): A96. http://dx.doi.org/10.1051/0004-6361/201425602.

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45

Piro, Luigi. "Multi-messenger science with Athena and Future Multi-messenger Observatories." Proceedings of the International Astronomical Union 16, S363 (2020): 135–48. http://dx.doi.org/10.1017/s1743921322002009.

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AbstractScientific synergies between Athena and some of the key multi-messenger facilities that should be operative concurrently with Athena are presented. These facilities include LIGO A+, Advanced Virgo+ and future detectors for ground-based observation of gravitational waves (GW), LISA for space-based observations of GW, IceCube and KM3NeT for neutrino observations, CTA for very high energy observations. Multimessenger synergy science themes discussed here include pressing issues in the field of Astrophysics, Cosmology and Fundamental physics such as: the central engine and jet physics in c

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46

Herbst, Konstantin, Andreas Bartenschlager, John Lee Grenfell, et al. "Impact of Cosmic Rays on Atmospheric Ion Chemistry and Spectral Transmission Features of TRAPPIST-1e." Astrophysical Journal 961, no. 2 (2024): 164. http://dx.doi.org/10.3847/1538-4357/ad0895.

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Abstract Ongoing observing projects like the James Webb Space Telescope and future missions offer the chance to characterize Earth-like exoplanetary atmospheres. Thereby, M dwarfs are preferred targets for transit observations, for example, due to their favorable planet–star contrast ratio. However, the radiation and particle environment of these cool stars could be far more extreme than what we know from the Sun. Thus, knowing the stellar radiation and particle environment and its possible influence on detectable biosignatures—in particular, signs of life like ozone and methane—is crucial to

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47

Hinton, J. A., and R. L. C. Starling. "High-energy emission from transients." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 371, no. 1992 (2013): 20120279. http://dx.doi.org/10.1098/rsta.2012.0279.

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Cosmic explosions dissipate energy into their surroundings on a very wide range of time scales: producing shock waves and associated particle acceleration. The historical culprits for the acceleration of the bulk of Galactic cosmic rays are supernova remnants: explosions on approximately 10 4 year time scales. Increasingly, however, time-variable emission points to rapid and efficient particle acceleration in a range of different astrophysical systems. Gamma-ray bursts have the shortest time scales, with inferred bulk Lorentz factors of approximately 1000 and photons emitted beyond 100 GeV, bu

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48

Spite, Monique, and François Spite. "Li isotopes in metal-poor halo dwarfs: a more and more complicated story." Proceedings of the International Astronomical Union 5, S268 (2009): 201–10. http://dx.doi.org/10.1017/s1743921310004138.

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AbstractThe nuclei of the lithium isotopes are fragile, easily destroyed, so that, at variance with most of the other elements, they cannot be formed in stars through steady hydrostatic nucleosynthesis.The 7Li isotope is synthesized during primordial nucleosynthesis in the first minutes after the Big Bang and later by cosmic rays, by novae and in pulsations of AGB stars (possibly also by the ν process). 6Li is mainly formed by cosmic rays. The oldest (most metal-deficient) warm galactic stars should retain the signature of these processes if, (as it had been often expected) lithium is not depl

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49

Gyngard, Frank, Sachiko Amari, Ernst Zinner, and Ulrich Ott. "Cosmic-Ray Exposure Ages of Large Presolar SiC Grains." Publications of the Astronomical Society of Australia 26, no. 3 (2009): 278–83. http://dx.doi.org/10.1071/as08037.

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AbstractAmong presolar SiC grains found in the Murchison carbonaceous meteorites (average size less than 0.5 μm) are very large grains, ranging in size up to 50 μm. We interpret 6Li excesses measured in eight of these grains as being the result of spallation reactions by Galactic cosmic rays during the time the grains spent in the interstellar medium before their incorporation into the meteorite. Derived interstellar exposure ages range from 40 My to 1 Gy, the highest values being consistent with theoretical expectations of interstellar grain lifetimes. Although six grains have almost identica

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Sun, Xulei, Shuying Zheng, Zhaodong Shi, Bing Liu, and Ruizhi Yang. "Low-Energy Cosmic Rays and Associated MeV Gamma-Ray Emissions in the Protoplanetary System." Universe 10, no. 8 (2024): 310. http://dx.doi.org/10.3390/universe10080310.

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Low-energy cosmic rays (LECRs) play a crucial role in the formation of planetary systems, and detecting and reconstructing the properties of early LECRs is essential for understanding the mechanisms of planetary system formation. Given that LECRs interact with the surrounding medium to produce nuclear de-excitation line emissions, which are gamma-ray emissions with energy mainly within 0.1–10 MeV and are unaffected by stellar wind modulation, these emissions can accurately reflect the properties of LECRs. This study introduces an innovative method for using gamma-ray emissions to infer LECR pr

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