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1. Identity statement
Reference TypeJournal Article
Sitemtc-m16.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier6qtX3pFwXQZsFDuKxG/GA7ft
Repositorysid.inpe.br/marciana/2005/06.27.17.01   (restricted access)
Last Update2005:06.27.03.00.00 (UTC) administrator
Metadata Repositorysid.inpe.br/marciana/2005/06.27.17.01.40
Metadata Last Update2018:06.05.01.21.34 (UTC) administrator
Secondary KeyINPE-12809-PRE/8099
ISSN0103-9733
Citation KeyMadsenSawaFernCeca:2004:ExSoCh
TitleExploration of solar chromosphere using high resolution spectroscopic observations
Year2004
MonthDec.
Access Date2024, Oct. 31
Secondary TypePRE PN
Number of Files1
Size482 KiB
2. Context
Author1 Madsen, F. R. H.
2 Sawant, Hanumant Shankar
3 Fernandes, Francisco Carlos Rocha
4 Cecatto, José Roberto
Resume Identifier1
2 8JMKD3MGP5W/3C9JHBU
3
4 8JMKD3MGP5W/3C9JHJB
Group1 DAS-INPE-MCT-BR
Affiliation1 Instituto Nacional de Pesquisas Espaciais, (INPE)
JournalBrazilian Journal of Physics
Volume34
Number4b
Pages1538-1541
History (UTC)2005-06-28 11:40:36 :: sergio -> administrator ::
2006-09-28 22:28:53 :: administrator -> sergio ::
2008-01-07 12:54:01 :: sergio -> administrator ::
2018-06-05 01:21:34 :: administrator -> marciana :: 2004
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
KeywordsCORONA
BSS
AbstractBrazilian Solar Spectroscope (BSS), operating in the frequency range of (1000 - 2500) MHz with high time and frequency resolutions, has observed various fine structures showing intensity variations as functions of time and frequency. Here we are reporting radio bursts observed by BSS, from August to October/2001, exhibiting fine structures with total duration of the order of 300 ms, covering a frequency range of similar to200 MHz. These characteristics are similar to those of the narrow band type III bursts observed above 1000 MHz. Hence these fine structures are variants of decimetric narrow band type III-like bursts. The fine structures observed exhibit variation of intensity as a function of frequency and curvatures in the frequency-time plane. These fine structures are explained as a propagation effect. We suggest that these structures are the signatures of the chromospheric density inhomogeneities lying in the line-of-sight path between the observer and the radio source. If the emitted frequencies are lower than the plasma frequency of the inhomogeneity, there will be absorption over a certain band, corresponding to the dimension of the inhomogeneity. The curved like structures are due to lower group velocities of the lower frequencies in the density inhomogeneities. The estimated scale sizes of the irregularities obtained are of the order of 10(1)-10(4) km. Thus an alternative method to total solar eclipse observation is suggested for investigations of chromospheric density irregularities..
AreaCEA
doc Directory Contentaccess
source Directory Contentthere are no files
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4. Conditions of access and use
Languageen
Target Fileexploration solar.pdf
User Groupadministrator
sergio
Visibilityshown
Copy HolderSID/SCD
Archiving Policydenypublisher denyfinaldraft12
Read Permissiondeny from all and allow from 150.163
5. Allied materials
Next Higher Units8JMKD3MGPCW/3ETR8EH
DisseminationWEBSCI; PORTALCAPES; SCIELO.
Host Collectionsid.inpe.br/banon/2003/08.15.17.40
6. Notes
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7. Description control
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