[svn-upgrade] Integrating new upstream version, jabref (2.3~beta1)
[debian/jabref.git] / src / java / tests / net / sf / jabref / imports / oai2.xml
1 <?xml version="1.0" encoding="UTF-8"?>
2 <OAI-PMH xmlns="http://www.openarchives.org/OAI/2.0/" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.openarchives.org/OAI/2.0/ http://www.openarchives.org/OAI/2.0/OAI-PMH.xsd">
3 <responseDate>2006-11-17T15:29:52Z</responseDate>
4 <request verb="GetRecord" identifier="oai:arXiv.org:hep-ph/0408155" metadataPrefix="arXiv">http://arXiv.org/oai2</request>
5 <GetRecord>
6 <record>
7 <header>
8  <identifier>oai:arXiv.org:hep-ph/0408155</identifier>
9  <datestamp>2005-09-18</datestamp>
10  <setSpec>physics:astro-ph</setSpec>
11  <setSpec>physics:hep-ph</setSpec>
12  <setSpec>physics:hep-th</setSpec>
13 </header>
14 <metadata>
15  <arXiv xmlns="http://arxiv.org/OAI/arXiv/" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://arxiv.org/OAI/arXiv/ http://arXiv.org/OAI/arXiv.xsd">
16  <id>hep-ph/0408155</id>
17  <authors>
18         <author><keyname>Giudice</keyname><forenames>G. F.</forenames></author>
19         <author><keyname>Riotto</keyname><forenames>A.</forenames></author>
20         <author><keyname>Zaffaroni</keyname><forenames>A.</forenames></author>
21         <author><keyname>López-Peña</keyname><forenames>J.</forenames></author>
22  </authors>
23  
24         <title>Heavy Particles from Inflation</title><categories>hep-ph astro-ph hep-th</categories><comments>23 pages</comments><report-no>CERN-PH-TH/2004-151</report-no><journal-ref>Nucl.Phys. B710 (2005) 511-525</journal-ref><doi>10.1016/j.nuclphysb.2004.12.037</doi><abstract>  We describe a simple and efficient mechanism by which very heavy particles
25 are copiously created from a primordial inflationary epoch. It works for scalar
26 fields which are massless or very light during inflation and acquire a large
27 mass right after the end of inflation. Such particles can exist in realistic
28 scenarios, as we illustrate with several examples in the context of both field
29 and string theory. Long-wavelength fluctuations of these fields are generated
30 during inflation with an almost scale-invariant spectrum and may give the
31 dominant contribution to the energy density of the heavy fields at late times.
32 Applications of our results to superheavy dark matter and leptogenesis are
33 discussed.
34 </abstract></arXiv>
35 </metadata>
36 </record>
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