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Meteor spectra studies started in the 1860s by means of the observations taken by A. Broad spectroscopy programmes were carried out in USA, Canada, the former USSR and Czechoslovakia (Ceplecha et al. New video techniques to study meteor spectra started to be used in the early 1970s (Hemenway et al.

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These elements were inserted inside two PVC tubes, which allow the whole set to be handled and moved without any relevant optical disturbances.The upper part of the tube is covered by 1-mm-thick float glass and with the same diameter as the tube, in order to correctly fit and being sealed with a special silicon cord for glass and exterior.2016), but the spectrographic equipment is limited to the spectral study of fireballs with visual apparent magnitude of − 4 and brighter.Light emitted by meteors during the ablation process in the terrestrial atmosphere allows us to study, by means of spectrographs, the chemical nature of their parent bodies.They serve as fastening and anchoring for the cameras and optical systems.

In the first experimental and test phase, adaptors with different height overlapping rings threaded between the CCD detector and the objective were placed to obtain the adequate focal length that would allow us to get sharp images.

The station allows the equipment to automatically start operating at sunset and being disconnected at sunrise on a daily basis.

We use two different spectrographs, with different optical configurations and CCD cameras, to attempt to get images with different fields of view and sensitivity for the same fireball.

Each of them is composed by a CCD camera with a wide-field telephoto lens, a holographic diffraction grating and adequate protection against weather (Fig. Both the CCDs and the lenses are different models, and thus, we have had to adopt two different settings in order to obtain two images simultaneously, with different spectral resolution each other.

To assemble all the elements that form the spectrograph, firstly, all elements were adjusted manually to obtain a precise optical focus and its stability.

Thus, the analysis of the spectrum of a given meteor can provide distinct information about the plasm, the ablation process and the chemical composition of the meteoroid (Borovička 1993, 1994a; Trigo-Rodríguez et al.