@MastersThesis{DelCiampo:1990:VaEmCe,
author = "Del Ciampo, Lineu Fernando",
title = "Varia{\c{c}}{\~a}o da emiss{\~a}o centim{\'e}trica de
V{\^e}nus segundo sua fase",
school = "Instituto Nacional de Pesquisas Espaciais (INPE)",
year = "1990",
address = "S{\~a}o Jos{\'e} dos Campos",
month = "1989-10-02",
keywords = "Planeta V{\^e}nus, radioemiss{\~a}o, ondas
cent{\'{\i}}metras.",
abstract = "A radioemiss{\~a}o do planeta V{\^e}nus, em comprimentos de onda
menores que 10 cm, apresenta algumas flutua{\c{c}}{\~o}es na
temperatura de luminosidade. As raz{\~o}es dessas
flutua{\c{c}}{\~o}es ainda s{\~a}o inconclusivas. Durante 1988,
V{\^e}nus estava relativamente mais perto da Terra que nos anos
precedentes e tamb{\'e}m apresentou mudan{\c{c}}as de
{\^a}ngulo de fase larga ao longo do ano. Esta
configura{\c{c}}{\~a}o orbital excepcional possibilitou ao
programa uma extensa s{\'e}rie de observa{\c{c}}{\~o}es com o
escopo de descobrir se h{\'a} algumas flutua{\c{c}}{\~o}es na
temperatura de luminosidade planet{\'a}ria associada {\`a} sua
fase. Para este programa foi usada a antena de 13,7 m do
Radiobservat{\'o}rio de Itapetinga, sendo as
observa{\c{c}}{\~o}es realizadas em 22 e 43 GHz. Este trabalho
apresenta os resultados observacionais da temperatura de
luminosidade de V{\^e}nus, de mar{\c{c}}o a outubro de 1988, que
mostra algumas flutua{\c{c}}{\~o}es nesta temperatura. Os
resultados das observa{\c{c}}{\~o}es sugerem que a
varia{\c{c}}{\~a}o da temperatura de luminosidade {\'a}
provavelmente devida ao {\^a}ngulo de fase do planeta. Esta
varia{\c{c}}{\~a}o de temperatura pode ser devida a
varia{\c{c}}{\~o}es na abund{\^a}ncia de S02, H20 e H2SO4
gasoso, que s{\~a}o os principais absorventes nesses comprimentos
de onda. ABSTRACT: The radio emission from the planet Venus, at
wavelengths smaller than 10 centimeter, presents some fluctuations
in the brightness temperature. The reasons for those fluctuations
are still inconclusive. During 1988, Venus was relatively closer
to the Earth than in the preceeding years and also presented large
phase angle changes along the year. This exceptional orbital
configuration allowed to program an extensive series of
observations with the scope of finding out if there is any
fluctuation in the planetary brightness temperature associated to
its phase. For this program it was used the 13.7 m antenna of the
Itapetinga Radio Observatory, being the observations carried out
at 22 GHz and 43 GHz. This work present the observacional results
of Venus brightness temperature, from March to October 1988, wich
shows some fluctuations in this temperature. The results of
observations suggest that the variation of the brightness
temperature is probably due to the phase angle of the planet. This
temperature variation may be due variations in the abundance of
SO2, 1120 and gaseous H 2SO 4 , wich are the main absorbers in
those wavelengths.",
committee = "Scalise J{\'u}nior, Eug{\^e}nio (presidente/orientador) and
Lazzaro, Daniela and Abraham, Zulema and Kotanyi, Christopher",
copyholder = "SID/SCD",
englishtitle = "x",
language = "pt",
pages = "97",
ibi = "8JMKD3MGP3W34P/3PTGGH8",
url = "http://urlib.net/ibi/8JMKD3MGP3W34P/3PTGGH8",
targetfile = "INPE-5122.pdf",
urlaccessdate = "28 mar. 2024"
}