Main characteristics of Solar System planets. Data are included in
the table, which includes non-standard EPN-TAP parameters. Data are
retrieved from Archinal et al 2018 (IAU report 2015,
2018CeMDA.130...22A) [radii] and Cox et al 2000 (Allen's astrophysical
quantities, 2000asqu.book.....C) [masses, heliocentric distances, and
rotation periods].
Pic du Midi de Bigorre in the French Pyrenees is the place where coronagraphic images were first realized, by Bernard Lyot in the 1930s. Since then, the solar instruments at Pic du Midi regularly provide images of the solar disc, solar prominences and solar corona.
Within this intermediate use case you learn about supernovae (see
also the tutorial “Distance to the Crab Nebula“,
ivo://edu.euro-vo.org/tutorials/08_m1_distance) and determine the
celestial coordinates of a just discovered candidate supernova on an
provided image without astrometric calibration. This use case provides
a glimpse of an activity that is representative of the practical tasks
that astronomers have to perform when they analyze data.
Data for numerical modeling of planetary atmospheres
Date:
12 Jun 2017 10:19:38
Publisher:
Instituto de Astrofisica de Andalucia-CSIC; INTA-CAB
Description:
Numerical modeling of composition and thermal balance of planetary
atmospheres requires a considerable amount of laboratory data. Among
them, the absorption cross sections in the UV range are needed both
for computing the heating in the atmosphere and the photodissociation
coefficients to initiate a rich disequilibrium chemistry. Prompted by
these needs in the community and by the sparse collection of data in
several other web pages (http://www.science-softcon.de/ or
http://satellite.mpic.de/spectral_atlas/index.html whose data depend
on some pre-processing before being ingested in these models), this
web page aims at providing the community with absorption cross
sections in the range 20 nm to 400 nm equally spaced every 0.2, 0.5
and 1.0 nm. Also, original data as appearing in the refereed journal
and the reference itself are downloadable.
The First Byurakan Survey (FBS) is the largest and the first systematic objective prism survey of the extragalactic sky. It covers 17,000 sq.deg. in the Northern sky together with a high galactic latitudes region in the Southern sky. The FBS has been carried out by B.E. Markarian, V.A. Lipovetski and J.A. Stepanian in 1965-1980 with the Byurakan Observatory 102/132/213 cm (40"/52"/84") Schmidt telescope using 1.5 deg. prism. Each FBS plate contains low-dispersion spectra of some 15,000-20,000 objects; the whole survey consists of about 20,000,000 objects.
Within this use case for high school students and adanced amateurs
you measure the linear distance of the Andromeda Galaxy following the
steps of the astronomers who first measured it, climbing an important
step of the so-called cosmic distance ladder. The use case requires
the identification of variable stars of the Cepheid class and the
determination of the relation between their period and their intrinsic
luminosity.
Within this use case you learn about supernovae, exploding or
exploded stars. In particular you will use information on the Crab
Nebula (the 1054 aD supernova registered by Chinese astronomers) to
derive its distance: an example of how some very important information
may be gained from very simple arguments and geometry.
