Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite
The precise measurement of the spectrum of protons, the most abundant component of the cosmic radiation, is necessary to understand the source and acceleration of cosmic rays in the Milky Way. This work reports the measurement of the cosmic ray proton fluxes with kinetic energies from 40 GeV to 100...
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| Veröffentlicht in: | Science advances 2019-09, Vol.5 (9), p.eaax3793-eaax3793 |
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| creator | An, Q Asfandiyarov, R Azzarello, P Bernardini, P Bi, X J Cai, M S Chang, J Chen, D Y Chen, H F Chen, J L Chen, W Cui, M Y Cui, T S Dai, H T D'Amone, A De Benedittis, A De Mitri, I Di Santo, M Ding, M Dong, T K Dong, Y F Dong, Z X Donvito, G Droz, D Duan, J L Duan, K K D'Urso, D Fan, R R Fan, Y Z Fang, F Feng, C Q Feng, L Fusco, P Gallo, V Gan, F J Gao, M Gargano, F Gong, K Gong, Y Z Guo, D Y Guo, J H Guo, X L Han, S X Hu, Y M Huang, G S Huang, X Y Huang, Y Y Ionica, M Jiang, W Jin, X Kong, J Lei, S J Li, S Li, W L Li, X Li, X Q Li, Y Liang, Y F Liang, Y M Liao, N H Liu, C M Liu, H Liu, J Liu, S B Liu, W Q Liu, Y Loparco, F Luo, C N Ma, M Ma, P X Ma, S Y Ma, T Ma, X Y Marsella, G Mazziotta, M N Mo, D Niu, X Y Pan, X Peng, W X Peng, X Y Qiao, R Rao, J N Salinas, M M Shang, G Z Shen, W H Shen, Z Q Shen, Z T Song, J X Su, H Su, M Sun, Z Y Surdo, A Teng, X J Tykhonov, A Vitillo, S Wang, C Wang, H Wang, H Y Wang, J Z Wang, L G |
| description | The precise measurement of the spectrum of protons, the most abundant component of the cosmic radiation, is necessary to understand the source and acceleration of cosmic rays in the Milky Way. This work reports the measurement of the cosmic ray proton fluxes with kinetic energies from 40 GeV to 100 TeV, with 2
/
years of data recorded by the DArk Matter Particle Explorer (DAMPE). This is the first time that an experiment directly measures the cosmic ray protons up to ~100 TeV with high statistics. The measured spectrum confirms the spectral hardening at ~300 GeV found by previous experiments and reveals a softening at ~13.6 TeV, with the spectral index changing from ~2.60 to ~2.85. Our result suggests the existence of a new spectral feature of cosmic rays at energies lower than the so-called knee and sheds new light on the origin of Galactic cosmic rays. |
| doi_str_mv | 10.1126/sciadv.aax3793 |
| format | Article |
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/
years of data recorded by the DArk Matter Particle Explorer (DAMPE). This is the first time that an experiment directly measures the cosmic ray protons up to ~100 TeV with high statistics. The measured spectrum confirms the spectral hardening at ~300 GeV found by previous experiments and reveals a softening at ~13.6 TeV, with the spectral index changing from ~2.60 to ~2.85. Our result suggests the existence of a new spectral feature of cosmic rays at energies lower than the so-called knee and sheds new light on the origin of Galactic cosmic rays.</description><identifier>ISSN: 2375-2548</identifier><identifier>EISSN: 2375-2548</identifier><identifier>DOI: 10.1126/sciadv.aax3793</identifier><identifier>PMID: 31799401</identifier><language>eng</language><publisher>United States: AAAS</publisher><subject>ASTRONOMY AND ASTROPHYSICS ; Physics ; SciAdv r-articles</subject><ispartof>Science advances, 2019-09, Vol.5 (9), p.eaax3793-eaax3793</ispartof><rights>Copyright © 2019 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works. Distributed under a Creative Commons Attribution NonCommercial License 4.0 (CC BY-NC).</rights><rights>Copyright © 2019 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works. 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0000000219391836</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://www.ncbi.nlm.nih.gov/pmc/articles/PMC6868675/pdf/$$EPDF$$P50$$Gpubmedcentral$$Hfree_for_read</linktopdf><linktohtml>$$Uhttps://www.ncbi.nlm.nih.gov/pmc/articles/PMC6868675/$$EHTML$$P50$$Gpubmedcentral$$Hfree_for_read</linktohtml><link.rule.ids>230,314,723,776,780,860,881,27901,27902,53766,53768</link.rule.ids><backlink>$$Uhttps://www.ncbi.nlm.nih.gov/pubmed/31799401$$D View this record in MEDLINE/PubMed$$Hfree_for_read</backlink><backlink>$$Uhttps://www.osti.gov/servlets/purl/1572843$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>An, Q</creatorcontrib><creatorcontrib>Asfandiyarov, R</creatorcontrib><creatorcontrib>Azzarello, P</creatorcontrib><creatorcontrib>Bernardini, P</creatorcontrib><creatorcontrib>Bi, X 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D</creatorcontrib><creatorcontrib>Niu, X Y</creatorcontrib><creatorcontrib>Pan, X</creatorcontrib><creatorcontrib>Peng, W X</creatorcontrib><creatorcontrib>Peng, X Y</creatorcontrib><creatorcontrib>Qiao, R</creatorcontrib><creatorcontrib>Rao, J N</creatorcontrib><creatorcontrib>Salinas, M M</creatorcontrib><creatorcontrib>Shang, G Z</creatorcontrib><creatorcontrib>Shen, W H</creatorcontrib><creatorcontrib>Shen, Z Q</creatorcontrib><creatorcontrib>Shen, Z T</creatorcontrib><creatorcontrib>Song, J X</creatorcontrib><creatorcontrib>Su, H</creatorcontrib><creatorcontrib>Su, M</creatorcontrib><creatorcontrib>Sun, Z Y</creatorcontrib><creatorcontrib>Surdo, A</creatorcontrib><creatorcontrib>Teng, X J</creatorcontrib><creatorcontrib>Tykhonov, A</creatorcontrib><creatorcontrib>Vitillo, S</creatorcontrib><creatorcontrib>Wang, C</creatorcontrib><creatorcontrib>Wang, H</creatorcontrib><creatorcontrib>Wang, H Y</creatorcontrib><creatorcontrib>Wang, J Z</creatorcontrib><creatorcontrib>Wang, L G</creatorcontrib><creatorcontrib>DAMPE Collaboration</creatorcontrib><creatorcontrib>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</creatorcontrib><title>Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite</title><title>Science advances</title><addtitle>Sci Adv</addtitle><description>The precise measurement of the spectrum of protons, the most abundant component of the cosmic radiation, is necessary to understand the source and acceleration of cosmic rays in the Milky Way. This work reports the measurement of the cosmic ray proton fluxes with kinetic energies from 40 GeV to 100 TeV, with 2
/
years of data recorded by the DArk Matter Particle Explorer (DAMPE). This is the first time that an experiment directly measures the cosmic ray protons up to ~100 TeV with high statistics. The measured spectrum confirms the spectral hardening at ~300 GeV found by previous experiments and reveals a softening at ~13.6 TeV, with the spectral index changing from ~2.60 to ~2.85. Our result suggests the existence of a new spectral feature of cosmic rays at energies lower than the so-called knee and sheds new light on the origin of Galactic cosmic rays.</description><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>Physics</subject><subject>SciAdv 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; Qiao, R ; Rao, J N ; Salinas, M M ; Shang, G Z ; Shen, W H ; Shen, Z Q ; Shen, Z T ; Song, J X ; Su, H ; Su, M ; Sun, Z Y ; Surdo, A ; Teng, X J ; Tykhonov, A ; Vitillo, S ; Wang, C ; Wang, H ; Wang, H Y ; Wang, J Z ; Wang, L G</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c417t-a976082dd5e9428fbd11f4de620014a781ce2e8b47b159238bedc9414f6748863</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>ASTRONOMY AND ASTROPHYSICS</topic><topic>Physics</topic><topic>SciAdv r-articles</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>An, Q</creatorcontrib><creatorcontrib>Asfandiyarov, R</creatorcontrib><creatorcontrib>Azzarello, P</creatorcontrib><creatorcontrib>Bernardini, P</creatorcontrib><creatorcontrib>Bi, X J</creatorcontrib><creatorcontrib>Cai, M S</creatorcontrib><creatorcontrib>Chang, J</creatorcontrib><creatorcontrib>Chen, D 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(LBNL), Berkeley, CA (United States)</creatorcontrib><collection>PubMed</collection><collection>CrossRef</collection><collection>MEDLINE - Academic</collection><collection>OSTI.GOV - Hybrid</collection><collection>OSTI.GOV</collection><collection>PubMed Central (Full Participant titles)</collection><jtitle>Science advances</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>An, Q</au><au>Asfandiyarov, R</au><au>Azzarello, P</au><au>Bernardini, P</au><au>Bi, X J</au><au>Cai, M S</au><au>Chang, J</au><au>Chen, D Y</au><au>Chen, H F</au><au>Chen, J L</au><au>Chen, W</au><au>Cui, M Y</au><au>Cui, T S</au><au>Dai, H T</au><au>D'Amone, A</au><au>De Benedittis, A</au><au>De Mitri, I</au><au>Di Santo, M</au><au>Ding, M</au><au>Dong, T K</au><au>Dong, Y F</au><au>Dong, Z X</au><au>Donvito, G</au><au>Droz, D</au><au>Duan, J L</au><au>Duan, K K</au><au>D'Urso, D</au><au>Fan, R R</au><au>Fan, Y Z</au><au>Fang, F</au><au>Feng, C Q</au><au>Feng, L</au><au>Fusco, P</au><au>Gallo, V</au><au>Gan, F J</au><au>Gao, M</au><au>Gargano, F</au><au>Gong, K</au><au>Gong, Y Z</au><au>Guo, D Y</au><au>Guo, J H</au><au>Guo, X L</au><au>Han, S X</au><au>Hu, Y M</au><au>Huang, G S</au><au>Huang, X Y</au><au>Huang, Y Y</au><au>Ionica, M</au><au>Jiang, W</au><au>Jin, X</au><au>Kong, J</au><au>Lei, S J</au><au>Li, S</au><au>Li, W L</au><au>Li, X</au><au>Li, X Q</au><au>Li, Y</au><au>Liang, Y F</au><au>Liang, Y M</au><au>Liao, N H</au><au>Liu, C M</au><au>Liu, H</au><au>Liu, J</au><au>Liu, S B</au><au>Liu, W Q</au><au>Liu, Y</au><au>Loparco, F</au><au>Luo, C N</au><au>Ma, M</au><au>Ma, P X</au><au>Ma, S Y</au><au>Ma, T</au><au>Ma, X Y</au><au>Marsella, G</au><au>Mazziotta, M N</au><au>Mo, D</au><au>Niu, X Y</au><au>Pan, X</au><au>Peng, W X</au><au>Peng, X Y</au><au>Qiao, R</au><au>Rao, J N</au><au>Salinas, M M</au><au>Shang, G Z</au><au>Shen, W H</au><au>Shen, Z Q</au><au>Shen, Z T</au><au>Song, J X</au><au>Su, H</au><au>Su, M</au><au>Sun, Z Y</au><au>Surdo, A</au><au>Teng, X J</au><au>Tykhonov, A</au><au>Vitillo, S</au><au>Wang, C</au><au>Wang, H</au><au>Wang, H Y</au><au>Wang, J Z</au><au>Wang, L G</au><aucorp>DAMPE Collaboration</aucorp><aucorp>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite</atitle><jtitle>Science advances</jtitle><addtitle>Sci Adv</addtitle><date>2019-09-01</date><risdate>2019</risdate><volume>5</volume><issue>9</issue><spage>eaax3793</spage><epage>eaax3793</epage><pages>eaax3793-eaax3793</pages><issn>2375-2548</issn><eissn>2375-2548</eissn><abstract>The precise measurement of the spectrum of protons, the most abundant component of the cosmic radiation, is necessary to understand the source and acceleration of cosmic rays in the Milky Way. This work reports the measurement of the cosmic ray proton fluxes with kinetic energies from 40 GeV to 100 TeV, with 2
/
years of data recorded by the DArk Matter Particle Explorer (DAMPE). This is the first time that an experiment directly measures the cosmic ray protons up to ~100 TeV with high statistics. The measured spectrum confirms the spectral hardening at ~300 GeV found by previous experiments and reveals a softening at ~13.6 TeV, with the spectral index changing from ~2.60 to ~2.85. Our result suggests the existence of a new spectral feature of cosmic rays at energies lower than the so-called knee and sheds new light on the origin of Galactic cosmic rays.</abstract><cop>United States</cop><pub>AAAS</pub><pmid>31799401</pmid><doi>10.1126/sciadv.aax3793</doi><orcidid>https://orcid.org/0000-0002-7667-3178</orcidid><orcidid>https://orcid.org/0000-0002-4666-9485</orcidid><orcidid>https://orcid.org/0000-0002-6316-1616</orcidid><orcidid>https://orcid.org/0000-0002-8937-4388</orcidid><orcidid>https://orcid.org/0000-0001-5704-5056</orcidid><orcidid>https://orcid.org/0000-0002-0263-3640</orcidid><orcidid>https://orcid.org/0000-0002-5924-3686</orcidid><orcidid>https://orcid.org/0000-0003-2908-7915</orcidid><orcidid>https://orcid.org/0000-0002-8215-4542</orcidid><orcidid>https://orcid.org/0000-0002-5778-8228</orcidid><orcidid>https://orcid.org/0000-0001-7398-0298</orcidid><orcidid>https://orcid.org/0000-0002-8547-9115</orcidid><orcidid>https://orcid.org/0000-0002-1173-5673</orcidid><orcidid>https://orcid.org/0000-0002-9383-2425</orcidid><orcidid>https://orcid.org/0000-0003-3210-9396</orcidid><orcidid>https://orcid.org/0000-0002-3439-957X</orcidid><orcidid>https://orcid.org/0000-0002-7357-0448</orcidid><orcidid>https://orcid.org/0000-0002-6631-9220</orcidid><orcidid>https://orcid.org/0000-0002-8966-6911</orcidid><orcidid>https://orcid.org/0000-0001-9325-4672</orcidid><orcidid>https://orcid.org/0000-0001-8275-5738</orcidid><orcidid>https://orcid.org/0000-0002-5055-6395</orcidid><orcidid>https://orcid.org/0000-0002-9019-5088</orcidid><orcidid>https://orcid.org/0000-0003-2715-589X</orcidid><orcidid>https://orcid.org/0000-0002-5656-6375</orcidid><orcidid>https://orcid.org/0000-0002-3155-6437</orcidid><orcidid>https://orcid.org/0000-0002-8665-1730</orcidid><orcidid>https://orcid.org/0000-0003-0427-0510</orcidid><orcidid>https://orcid.org/0000-0002-5894-3429</orcidid><orcidid>https://orcid.org/000000017655389X</orcidid><orcidid>https://orcid.org/0000000266319220</orcidid><orcidid>https://orcid.org/0000000193254672</orcidid><orcidid>https://orcid.org/0000000257350082</orcidid><orcidid>https://orcid.org/0000000293832425</orcidid><orcidid>https://orcid.org/0000000257788228</orcidid><orcidid>https://orcid.org/0000000349637275</orcidid><orcidid>https://orcid.org/0000000329087915</orcidid><orcidid>https://orcid.org/0000000256566375</orcidid><orcidid>https://orcid.org/0000000263161616</orcidid><orcidid>https://orcid.org/000000023439957X</orcidid><orcidid>https://orcid.org/0000000157045056</orcidid><orcidid>https://orcid.org/0000000250556395</orcidid><orcidid>https://orcid.org/0000000297585476</orcidid><orcidid>https://orcid.org/0000000211735673</orcidid><orcidid>https://orcid.org/0000000285479115</orcidid><orcidid>https://orcid.org/0000000231556437</orcidid><orcidid>https://orcid.org/0000000332109396</orcidid><orcidid>https://orcid.org/0000000289666911</orcidid><orcidid>https://orcid.org/0000000304270510</orcidid><orcidid>https://orcid.org/0000000282154542</orcidid><orcidid>https://orcid.org/0000000182755738</orcidid><orcidid>https://orcid.org/0000000173980298</orcidid><orcidid>https://orcid.org/0000000258943429</orcidid><orcidid>https://orcid.org/0000000196269319</orcidid><orcidid>https://orcid.org/000000021345092X</orcidid><orcidid>https://orcid.org/0000000313077181</orcidid><orcidid>https://orcid.org/0000000290195088</orcidid><orcidid>https://orcid.org/000000032715589X</orcidid><orcidid>https://orcid.org/0000000289374388</orcidid><orcidid>https://orcid.org/0000000273570448</orcidid><orcidid>https://orcid.org/0000000348913186</orcidid><orcidid>https://orcid.org/0000000286651730</orcidid><orcidid>https://orcid.org/0000000276673178</orcidid><orcidid>https://orcid.org/0000000259243686</orcidid><orcidid>https://orcid.org/0000000202633640</orcidid><orcidid>https://orcid.org/0000000246669485</orcidid><orcidid>https://orcid.org/0000000321415208</orcidid><orcidid>https://orcid.org/0000000336168318</orcidid><orcidid>https://orcid.org/0000000219391836</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 2375-2548 |
| ispartof | Science advances, 2019-09, Vol.5 (9), p.eaax3793-eaax3793 |
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| language | eng |
| recordid | cdi_pubmedcentral_primary_oai_pubmedcentral_nih_gov_6868675 |
| source | DOAJ Directory of Open Access Journals; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; PubMed Central |
| subjects | ASTRONOMY AND ASTROPHYSICS Physics SciAdv r-articles |
| title | Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite |
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