Seesaw Mechanism Confronting PAMELA in S_4 Flavor Symmetric Extra U(1) Model
We study cosmic-ray anomaly observed by PAMELA based on E_6 inspired extra U(1) model with S_4 flavor symmetry. In our model, the lightest flavon has very long lifetime of O(10^18) second which is longer than the age of the universe, but not long enough to explain the PAMELA result O(10^26) sec. Suc...
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| creator | Daikoku, Yasuhiro Okada, Hiroshi Toma, Takashi |
| description | We study cosmic-ray anomaly observed by PAMELA based on E_6 inspired extra
U(1) model with S_4 flavor symmetry. In our model, the lightest flavon has very
long lifetime of O(10^18) second which is longer than the age of the universe,
but not long enough to explain the PAMELA result O(10^26) sec. Such a situation
could be avoidable by considering that the flavon is not the dominant component
of dark matters. However non-thermalizing the flavon is needed to obtain proper
relic density. This relates reheating temperature of the universe with seesaw
mass scale. If we assume this flavon is a particle decaying into positron (or
electron), the seesaw mass scale is constrained by reheating temperature. Thus
we find an interesting result that the allowed region is around O(10^12) GeV,
which is consistent with our original result. |
| doi_str_mv | 10.48550/arxiv.1010.4963 |
| format | Article |
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U(1) model with S_4 flavor symmetry. In our model, the lightest flavon has very
long lifetime of O(10^18) second which is longer than the age of the universe,
but not long enough to explain the PAMELA result O(10^26) sec. Such a situation
could be avoidable by considering that the flavon is not the dominant component
of dark matters. However non-thermalizing the flavon is needed to obtain proper
relic density. This relates reheating temperature of the universe with seesaw
mass scale. If we assume this flavon is a particle decaying into positron (or
electron), the seesaw mass scale is constrained by reheating temperature. Thus
we find an interesting result that the allowed region is around O(10^12) GeV,
which is consistent with our original result.</description><identifier>DOI: 10.48550/arxiv.1010.4963</identifier><language>eng</language><subject>Physics - High Energy Astrophysical Phenomena ; Physics - High Energy Physics - Phenomenology</subject><creationdate>2010-10</creationdate><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,885</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/1010.4963$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.48550/arXiv.1010.4963$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Daikoku, Yasuhiro</creatorcontrib><creatorcontrib>Okada, Hiroshi</creatorcontrib><creatorcontrib>Toma, Takashi</creatorcontrib><title>Seesaw Mechanism Confronting PAMELA in S_4 Flavor Symmetric Extra U(1) Model</title><description>We study cosmic-ray anomaly observed by PAMELA based on E_6 inspired extra
U(1) model with S_4 flavor symmetry. In our model, the lightest flavon has very
long lifetime of O(10^18) second which is longer than the age of the universe,
but not long enough to explain the PAMELA result O(10^26) sec. Such a situation
could be avoidable by considering that the flavon is not the dominant component
of dark matters. However non-thermalizing the flavon is needed to obtain proper
relic density. This relates reheating temperature of the universe with seesaw
mass scale. If we assume this flavon is a particle decaying into positron (or
electron), the seesaw mass scale is constrained by reheating temperature. Thus
we find an interesting result that the allowed region is around O(10^12) GeV,
which is consistent with our original result.</description><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Physics - High Energy Physics - Phenomenology</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2010</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNotz79LxDAYxvEsDnK6Ox0ZdeiZXH40HUvpqdCi0HMub5s3GmhTSct5999L1emB7_DAh5A7znbSKMUeIZ79acfZGjItrknVIM7wTWvsPyH4eaTFFFycwuLDB33L67LKqQ-0aSU9DHCaIm0u44hL9D0tz0sE-n7PH2g9WRxuyJWDYcbb_92Q46E8Fs9J9fr0UuRVAlqJRBupNDMA4DLHRMd7bi2yTkumrJVdqo0wnUBmncpEbzjLwKZcpmaPRiIXG7L9u_3VtF_RjxAv7apqV5X4ARU9RVY</recordid><startdate>20101024</startdate><enddate>20101024</enddate><creator>Daikoku, Yasuhiro</creator><creator>Okada, Hiroshi</creator><creator>Toma, Takashi</creator><scope>GOX</scope></search><sort><creationdate>20101024</creationdate><title>Seesaw Mechanism Confronting PAMELA in S_4 Flavor Symmetric Extra U(1) Model</title><author>Daikoku, Yasuhiro ; Okada, Hiroshi ; Toma, Takashi</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a653-6845608aaaf9f03b1c1dde0b6405dd4b76838b3e0df593c8109ad714782e84e13</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2010</creationdate><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Physics - High Energy Physics - Phenomenology</topic><toplevel>online_resources</toplevel><creatorcontrib>Daikoku, Yasuhiro</creatorcontrib><creatorcontrib>Okada, Hiroshi</creatorcontrib><creatorcontrib>Toma, Takashi</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Daikoku, Yasuhiro</au><au>Okada, Hiroshi</au><au>Toma, Takashi</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Seesaw Mechanism Confronting PAMELA in S_4 Flavor Symmetric Extra U(1) Model</atitle><date>2010-10-24</date><risdate>2010</risdate><abstract>We study cosmic-ray anomaly observed by PAMELA based on E_6 inspired extra
U(1) model with S_4 flavor symmetry. In our model, the lightest flavon has very
long lifetime of O(10^18) second which is longer than the age of the universe,
but not long enough to explain the PAMELA result O(10^26) sec. Such a situation
could be avoidable by considering that the flavon is not the dominant component
of dark matters. However non-thermalizing the flavon is needed to obtain proper
relic density. This relates reheating temperature of the universe with seesaw
mass scale. If we assume this flavon is a particle decaying into positron (or
electron), the seesaw mass scale is constrained by reheating temperature. Thus
we find an interesting result that the allowed region is around O(10^12) GeV,
which is consistent with our original result.</abstract><doi>10.48550/arxiv.1010.4963</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Physics - High Energy Astrophysical Phenomena Physics - High Energy Physics - Phenomenology |
| title | Seesaw Mechanism Confronting PAMELA in S_4 Flavor Symmetric Extra U(1) Model |
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