Proton-helium spectral anomaly as a signature of cosmic ray accelerator
The much-anticipated proof of cosmic ray (CR) acceleration in supernova remnants must hinge on the full consistency of acceleration theory with the observations; direct proof is impossible because of CR-orbit scrambling. Recent observations indicate deviations between helium and proton CR rigidity s...
Saved in:
Published in | Physical review letters Vol. 108; no. 8; p. 081104 |
---|---|
Main Authors | , , |
Format | Journal Article |
Language | English |
Published |
United States
24.02.2012
|
Online Access | Get more information |
Cover
Loading…
Abstract | The much-anticipated proof of cosmic ray (CR) acceleration in supernova remnants must hinge on the full consistency of acceleration theory with the observations; direct proof is impossible because of CR-orbit scrambling. Recent observations indicate deviations between helium and proton CR rigidity spectra inconsistent with the theory. By considering an initial (injection) phase of the diffusive shock acceleration, where elemental similarity does not apply, we demonstrate that the spectral difference is, in fact, a unique signature of the acceleration mechanism. Collisionless shocks inject more He(2+) when they are stronger and so produce harder He(2+) spectra. The injection bias is due to Alfvén waves driven by the more abundant protons, so the He(2+) ions are harder to trap by these waves. By fitting the p/He ratio to the PAMELA data, we bolster the diffusive shock acceleration case for resolving the century-old mystery of CR origin. |
---|---|
AbstractList | The much-anticipated proof of cosmic ray (CR) acceleration in supernova remnants must hinge on the full consistency of acceleration theory with the observations; direct proof is impossible because of CR-orbit scrambling. Recent observations indicate deviations between helium and proton CR rigidity spectra inconsistent with the theory. By considering an initial (injection) phase of the diffusive shock acceleration, where elemental similarity does not apply, we demonstrate that the spectral difference is, in fact, a unique signature of the acceleration mechanism. Collisionless shocks inject more He(2+) when they are stronger and so produce harder He(2+) spectra. The injection bias is due to Alfvén waves driven by the more abundant protons, so the He(2+) ions are harder to trap by these waves. By fitting the p/He ratio to the PAMELA data, we bolster the diffusive shock acceleration case for resolving the century-old mystery of CR origin. |
Author | Diamond, P H Malkov, M A Sagdeev, R Z |
Author_xml | – sequence: 1 givenname: M A surname: Malkov fullname: Malkov, M A organization: CASS and Department of Physics, University of California, San Diego, La Jolla, California 92093, USA – sequence: 2 givenname: P H surname: Diamond fullname: Diamond, P H – sequence: 3 givenname: R Z surname: Sagdeev fullname: Sagdeev, R Z |
BackLink | https://www.ncbi.nlm.nih.gov/pubmed/22463513$$D View this record in MEDLINE/PubMed |
BookMark | eNo1j9tKAzEURYMo9qK_UPIDU3OSzKWPUrQKBX3Q53LmzIkdmZkMSUbo31tRnzbsBZu1F-Jy8AMLsQK1BlDmbjyeYuCvjlNag6rWqjrX9kLMQZWbrASwM7GI8VMpBbqorsVMa1uYHMxc7F6DT37Ijty1Uy_jyJQCdhIH32N3khglyth-DJimwNI7ST72LcmAZ0jEHQdMPtyIK4dd5Nu_XIr3x4e37VO2f9k9b-_3GdkcUgZNpZkUuQYbKsg5KH6UOLcOTa4sO22s2lBdF9ho4xqoqDRYU6FKu3G1XorV7-441T03hzG0PYbT4f-R_gbH9lI1 |
CitedBy_id | crossref_primary_10_1016_j_physrep_2014_06_003 crossref_primary_10_1103_PhysRevD_86_114024 crossref_primary_10_1088_1742_6596_409_1_012052 crossref_primary_10_3847_1538_4357_aa68e4 crossref_primary_10_1063_1_4945649 crossref_primary_10_1063_1_4928941 crossref_primary_10_1103_PhysRevD_92_063001 crossref_primary_10_1103_PhysRevD_94_063006 crossref_primary_10_1016_j_asr_2017_04_019 crossref_primary_10_1016_j_nuclphysbps_2018_07_004 crossref_primary_10_1142_S0218271814300134 crossref_primary_10_3847_1538_4357_aaef39 crossref_primary_10_1103_PhysRevLett_128_131103 crossref_primary_10_1103_PhysRevD_93_083001 crossref_primary_10_1103_PhysRevD_99_103023 crossref_primary_10_1103_PhysRevD_103_123010 crossref_primary_10_3847_1538_4357_ac7049 crossref_primary_10_1088_1742_6596_1336_1_012010 crossref_primary_10_1051_0004_6361_201321202 crossref_primary_10_1016_j_nuclphysbps_2013_05_023 crossref_primary_10_1007_s40766_020_00007_2 crossref_primary_10_1103_PhysRevLett_129_101102 crossref_primary_10_1142_S0218271819300222 crossref_primary_10_1103_PhysRevLett_126_241101 crossref_primary_10_1016_j_ppnp_2020_103765 crossref_primary_10_1088_1475_7516_2019_12_007 crossref_primary_10_1088_1674_4527_15_1_002 crossref_primary_10_1134_S1063780X15080048 crossref_primary_10_1103_PhysRevD_94_123019 crossref_primary_10_1103_PhysRevD_97_023015 crossref_primary_10_1103_PhysRevLett_130_171002 crossref_primary_10_1063_1_4737584 crossref_primary_10_1051_0004_6361_201526877 crossref_primary_10_3847_1538_4357_abbe05 crossref_primary_10_1088_1674_4527_acdabd crossref_primary_10_1103_PhysRevLett_115_211101 crossref_primary_10_1016_j_physletb_2017_02_035 crossref_primary_10_1103_PhysRevD_96_023006 crossref_primary_10_1088_2041_8205_815_1_L1 crossref_primary_10_1103_PhysRevLett_125_251102 crossref_primary_10_3847_2041_8213_aa7de1 crossref_primary_10_1093_mnras_stac470 crossref_primary_10_1103_PhysRevD_105_103033 crossref_primary_10_3847_1538_4357_ac22fe crossref_primary_10_1088_1475_7516_2013_07_001 crossref_primary_10_1088_1475_7516_2023_02_007 crossref_primary_10_1016_j_nima_2013_12_028 crossref_primary_10_1016_j_nuclphysbps_2018_07_023 crossref_primary_10_3847_1538_4365_aba901 crossref_primary_10_1016_j_physrep_2020_09_003 crossref_primary_10_1007_s12043_015_1157_7 crossref_primary_10_1103_PhysRevD_94_123007 crossref_primary_10_1051_epjconf_20147100115 crossref_primary_10_1103_PhysRevD_92_081301 crossref_primary_10_1016_j_astropartphys_2012_09_007 crossref_primary_10_1103_PhysRevLett_122_181102 crossref_primary_10_1016_j_asr_2016_10_024 crossref_primary_10_1134_S1063780X16070072 crossref_primary_10_3847_1538_4357_aafdae crossref_primary_10_3389_fspas_2022_1044225 crossref_primary_10_1088_2041_8205_803_2_L15 |
ContentType | Journal Article |
DBID | NPM |
DOI | 10.1103/physrevlett.108.081104 |
DatabaseName | PubMed |
DatabaseTitle | PubMed |
DatabaseTitleList | PubMed |
Database_xml | – sequence: 1 dbid: NPM name: PubMed url: https://proxy.k.utb.cz/login?url=http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?db=PubMed sourceTypes: Index Database |
DeliveryMethod | no_fulltext_linktorsrc |
Discipline | Physics |
EISSN | 1079-7114 |
ExternalDocumentID | 22463513 |
Genre | Journal Article |
GroupedDBID | --- -DZ -~X 123 2-P 29O 3MX 5VS 85S ACBEA ACGFO ACNCT AENEX AEQTI AFFNX AFGMR AGDNE AJQPL ALMA_UNASSIGNED_HOLDINGS APKKM AUAIK CS3 D0L DU5 EBS EJD F5P MVM N9A NPBMV NPM P0- P2P ROL S7W SJN TN5 UBE UCJ VQA WH7 XOL XSW YNT ZPR ~02 |
ID | FETCH-LOGICAL-c451t-1d82ec0cfdadc6cff161268e54fa3504ef23409cbb6ad23fd18c73abc60749fb2 |
IngestDate | Sat Sep 28 07:49:58 EDT 2024 |
IsDoiOpenAccess | false |
IsOpenAccess | true |
IsPeerReviewed | true |
IsScholarly | true |
Issue | 8 |
Language | English |
LinkModel | OpenURL |
MergedId | FETCHMERGED-LOGICAL-c451t-1d82ec0cfdadc6cff161268e54fa3504ef23409cbb6ad23fd18c73abc60749fb2 |
OpenAccessLink | https://link.aps.org/accepted/10.1103/PhysRevLett.108.081104 |
PMID | 22463513 |
ParticipantIDs | pubmed_primary_22463513 |
PublicationCentury | 2000 |
PublicationDate | 2012-02-24 |
PublicationDateYYYYMMDD | 2012-02-24 |
PublicationDate_xml | – month: 02 year: 2012 text: 2012-02-24 day: 24 |
PublicationDecade | 2010 |
PublicationPlace | United States |
PublicationPlace_xml | – name: United States |
PublicationTitle | Physical review letters |
PublicationTitleAlternate | Phys Rev Lett |
PublicationYear | 2012 |
SSID | ssj0001268 |
Score | 2.4299445 |
Snippet | The much-anticipated proof of cosmic ray (CR) acceleration in supernova remnants must hinge on the full consistency of acceleration theory with the... |
SourceID | pubmed |
SourceType | Index Database |
StartPage | 081104 |
Title | Proton-helium spectral anomaly as a signature of cosmic ray accelerator |
URI | https://www.ncbi.nlm.nih.gov/pubmed/22463513 |
Volume | 108 |
hasFullText | |
inHoldings | 1 |
isFullTextHit | |
isPrint | |
link | http://utb.summon.serialssolutions.com/2.0.0/link/0/eLvHCXMwnV1ZT-MwELY4tBIvCFiWG_mBN5RuDufoI-IUEgjtgsQbsp3xgmgb1BYk-PXM2E4bjkXAS1TFTeT4GzufJ_PNMLYFeWQSFUMg0jwMRBJrO6WCuATRpvwkIiWB88lpdnQhji_Ty4bimtQlQ9XST-_qSr6DKp5DXEkl-wVkRzfFE_gb8cUjIozHT2F81q-oAvA1dG7uu9tWNNm32v-qKzuPVEJGblOAhk3e6QLIBxQL35fYqDW-cexH9iZBPatx85qWjpX7jIj3iezcVg_Wizr2gu7dUMkiR0jHYoe_8l8JYP_7x3__8N4FCtOIAydqboFbEcO8HeSRU3qOlsywaNhG0VgAkWH4esJv1-aQckSQwwafgHpP8Y2ttxfgGN91LWKU7C5JnVb149ZXObPrpkk2mRe07p2SD2em9rxlhdeKY5d-v98hShLtb_Jqw2GJx_kcm_U7Br7j4J9nE9BbYD8cToOf7PCFEfDaCLg3Ai4HXPKREfDKcGcEHI2AN4xgkV0c7J_vHgW-OkagRRoNg6gsYtChNqUsdaaNQe6OTwapMDJJQwEmTnDzrpXKZBknpowKnSdS6QxZY9uo-Beb6lU9WGYc8kIXoJG7ylAoN0lVkoOUgAQwMytsyY3A1Z1LgXJVj83qf1vW2MzYntbZtME5BxtI4IZq0-LxDM93RmA |
link.rule.ids | 786 |
linkProvider | National Library of Medicine |
openUrl | ctx_ver=Z39.88-2004&ctx_enc=info%3Aofi%2Fenc%3AUTF-8&rfr_id=info%3Asid%2Fsummon.serialssolutions.com&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.atitle=Proton-helium+spectral+anomaly+as+a+signature+of+cosmic+ray+accelerator&rft.jtitle=Physical+review+letters&rft.au=Malkov%2C+M+A&rft.au=Diamond%2C+P+H&rft.au=Sagdeev%2C+R+Z&rft.date=2012-02-24&rft.eissn=1079-7114&rft.volume=108&rft.issue=8&rft.spage=081104&rft_id=info:doi/10.1103%2Fphysrevlett.108.081104&rft_id=info%3Apmid%2F22463513&rft_id=info%3Apmid%2F22463513&rft.externalDocID=22463513 |