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Assays to Detect UV-reflecting Structures and Determine their Importance in Mate Preference using the Sailfin Molly Poecilia latipinna

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Mariner 9 ultraviolet spectrometer experiment: stellar observations.

C F Lillie, R C Bohlin, M R Molnar

Science (New York, N.Y.)

|January 21, 1972

Summary

Ultraviolet spectra of early-type stars reveal key elemental lines. Mariner 9 data show energy distributions approximately 20% lower than previous observations, impacting stellar astrophysics research.

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Molecular Beam Mass Spectrometry With Tunable Vacuum Ultraviolet (VUV) Synchrotron Radiation

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Published on: October 30, 2012

Area of Science:

Astronomy and Astrophysics
Stellar Spectroscopy

Background:

Early-type stars are crucial for understanding stellar evolution and galactic composition.
Ultraviolet (UV) spectroscopy provides unique insights into stellar atmospheres and compositions.

Purpose of the Study:

To obtain photoelectric spectra of early-type stars in the 1100-2000 angstrom range.
To identify prominent spectral lines and analyze the absolute energy distribution of these stars.

Main Methods:

Utilized the Mariner 9 ultraviolet spectrometer to capture stellar spectra.
Focused on the 1100-2000 angstrom wavelength region.

Main Results:

Successfully identified resonance lines of Hydrogen I (H I), Silicon IV (Si IV), and Carbon IV (C IV).
Detected spectral features from Carbon II (C II), Carbon III (C III), Silicon III (Si III), Iron II (Fe II), and Nitrogen IV (N IV).
Derived absolute energy distributions that were approximately 20% lower than those obtained by OAO-2 in the 1200-2000 angstrom range.

Conclusions:

The study provides valuable UV spectral data for early-type stars.
Discrepancies in energy distribution compared to previous missions warrant further investigation into observational methods and calibration.