000612989 001__ 612989
000612989 005__ 20250723105628.0
000612989 0247_ $$2doi$$a10.1051/0004-6361/202451880
000612989 0247_ $$2ISSN$$a0004-6361
000612989 0247_ $$2ISSN$$a1432-0746
000612989 0247_ $$2datacite_doi$$a10.3204/PUBDB-2024-05495
000612989 0247_ $$2altmetric$$aaltmetric:175071232
000612989 0247_ $$2WOS$$aWOS:001457679200008
000612989 0247_ $$2openalex$$aopenalex:W4408397952
000612989 037__ $$aPUBDB-2024-05495
000612989 041__ $$aEnglish
000612989 082__ $$a520
000612989 1001_ $$0P:(DE-HGF)0$$aLópez-Coto, Rubén$$b0$$eCorresponding author
000612989 245__ $$aCosmic Ray bubbles from nova super remnants and their contribution to local cosmic ray spectra
000612989 260__ $$aLes Ulis$$bEDP Sciences$$c2025
000612989 3367_ $$2DRIVER$$aarticle
000612989 3367_ $$2DataCite$$aOutput Types/Journal article
000612989 3367_ $$0PUB:(DE-HGF)16$$2PUB:(DE-HGF)$$aJournal Article$$bjournal$$mjournal$$s1744372450_218621
000612989 3367_ $$2BibTeX$$aARTICLE
000612989 3367_ $$2ORCID$$aJOURNAL_ARTICLE
000612989 3367_ $$00$$2EndNote$$aJournal Article
000612989 520__ $$aContext. Several new phenomena have arisen in the area of study of the repeating thermonuclear explosions called novae. For example, recurrent novae have been proven to be efficient cosmic ray hadronic accelerators thanks to the recent observations of RS Ophiuchi by different γ-ray instruments. Novae have also been demonstrated to have the ability to carve large cavities into the interstellar medium (ISM), with parallels with the remnants of supernovae.Aims. Our aims are to calculate the effects of novae on their surrounding media, and the distances over which these effects dominate over the average quantities that are measured in the ISM.Methods. We calculated the filling factor of novae and their contribution to cosmic ray fluxes using cosmic ray propagation codes. To limit the atomic density of the ISM surrounding the region of RS Oph, we used Fermi-LAT observations of the region.Results. The filling factor of novae in the Galaxy is not significant under all assumptions done in the paper. They do not dominate over the local cosmic ray fluxes, even at the lowest energies, for distances larger than a few parsecs. The particle density of the ISM surrounding them is, however, very much modified, being lowered by more than one order of magnitude with respect to galactic averages, confirming estimates done using other observatories.Conclusions. Even though at global galactic distances, novae do not seem to be dominating cosmic ray transport, they have the power to modify the conditions of their surrounding ISM over parsec distances. 
000612989 536__ $$0G:(DE-HGF)POF4-613$$a613 - Matter and Radiation from the Universe (POF4-613)$$cPOF4-613$$fPOF IV$$x0
000612989 588__ $$aDataset connected to CrossRef, Journals: bib-pubdb1.desy.de
000612989 693__ $$0EXP:(DE-H253)Fermi-20170101$$5EXP:(DE-H253)Fermi-20170101$$eThe Fermi Large Area Telescope$$x0
000612989 7001_ $$0P:(DE-HGF)0$$aGreen, David$$b1
000612989 7001_ $$0P:(DE-HGF)0$$aMéndez-Gallego, Javier$$b2
000612989 7001_ $$0P:(DE-H253)PIP1085234$$ade Ona Wilhelmi, Emma Maria$$b3
000612989 773__ $$0PERI:(DE-600)1458466-9$$a10.1051/0004-6361/202451880$$gVol. 696, p. A24 -$$pA24 $$tAstronomy and astrophysics$$v696$$x0004-6361$$y2025
000612989 8564_ $$uhttps://bib-pubdb1.desy.de/record/612989/files/HTML-Approval_of_scientific_publication.html
000612989 8564_ $$uhttps://bib-pubdb1.desy.de/record/612989/files/PDF-Approval_of_scientific_publication.pdf
000612989 8564_ $$uhttps://bib-pubdb1.desy.de/record/612989/files/aa51880-24.pdf$$yOpenAccess
000612989 8564_ $$uhttps://bib-pubdb1.desy.de/record/612989/files/aa51880-24.pdf?subformat=pdfa$$xpdfa$$yOpenAccess
000612989 909CO $$ooai:bib-pubdb1.desy.de:612989$$pdnbdelivery$$pdriver$$pVDB$$popen_access$$popenaire
000612989 9101_ $$0I:(DE-588b)2008985-5$$6P:(DE-H253)PIP1085234$$aDeutsches Elektronen-Synchrotron$$b3$$kDESY
000612989 9131_ $$0G:(DE-HGF)POF4-613$$1G:(DE-HGF)POF4-610$$2G:(DE-HGF)POF4-600$$3G:(DE-HGF)POF4$$4G:(DE-HGF)POF$$aDE-HGF$$bForschungsbereich Materie$$lMatter and the Universe$$vMatter and Radiation from the Universe$$x0
000612989 9141_ $$y2025
000612989 915__ $$0StatID:(DE-HGF)0200$$2StatID$$aDBCoverage$$bSCOPUS$$d2024-12-31
000612989 915__ $$0StatID:(DE-HGF)0300$$2StatID$$aDBCoverage$$bMedline$$d2024-12-31
000612989 915__ $$0LIC:(DE-HGF)CCBY4$$2HGFVOC$$aCreative Commons Attribution CC BY 4.0
000612989 915__ $$0StatID:(DE-HGF)0600$$2StatID$$aDBCoverage$$bEbsco Academic Search$$d2024-12-31
000612989 915__ $$0StatID:(DE-HGF)1150$$2StatID$$aDBCoverage$$bCurrent Contents - Physical, Chemical and Earth Sciences$$d2024-12-31
000612989 915__ $$0StatID:(DE-HGF)9905$$2StatID$$aIF >= 5$$bASTRON ASTROPHYS : 2022$$d2024-12-31
000612989 915__ $$0StatID:(DE-HGF)0150$$2StatID$$aDBCoverage$$bWeb of Science Core Collection$$d2024-12-31
000612989 915__ $$0StatID:(DE-HGF)0113$$2StatID$$aWoS$$bScience Citation Index Expanded$$d2024-12-31
000612989 915__ $$0StatID:(DE-HGF)0510$$2StatID$$aOpenAccess
000612989 915__ $$0StatID:(DE-HGF)0030$$2StatID$$aPeer Review$$bASC$$d2024-12-31
000612989 915__ $$0StatID:(DE-HGF)0100$$2StatID$$aJCR$$bASTRON ASTROPHYS : 2022$$d2024-12-31
000612989 915__ $$0StatID:(DE-HGF)0160$$2StatID$$aDBCoverage$$bEssential Science Indicators$$d2024-12-31
000612989 915__ $$0StatID:(DE-HGF)0199$$2StatID$$aDBCoverage$$bClarivate Analytics Master Journal List$$d2024-12-31
000612989 9201_ $$0I:(DE-H253)Z_HESS-20210408$$kZ_HESS$$lHigh Energy Steroscopic System$$x0
000612989 980__ $$ajournal
000612989 980__ $$aVDB
000612989 980__ $$aUNRESTRICTED
000612989 980__ $$aI:(DE-H253)Z_HESS-20210408
000612989 9801_ $$aFullTexts