Development of a program of radiopaque lesions images via radiographic cases for active learning in oral medicine

Through the creation of this project in English, we have made a file of radiographic images that will be used by third year dental students in order to improve the practical teaching part of the subject of Oral Medicine, essentially by incorporating these files to the Virtual Campus. We have selected the most representative radiopaque radiographic images studied in pathology lectures given. We have prepared a file with 59 radiopaque radiographic images. These lesions have been divided according to their relationship and number with the tooth, into the following groups: “Anatomic radiopacities”, “Periapical radiopacities”, “Solitary radiopacities not necessarily contacting teeth”,“Multiple separate radiopacities”, and “Generalized radiopacities”. We created 4 flowcharts synthesizing the mayor explanatory bases of each pathological process in relation to other pathologies within each location. We have focused primarily in those clinical and radiographic features that can help us differentiate one pathology from another. We believe that by giving the student a knowledge base through each flowchart, as well as provide clinical cases, will start their curiosity to seek new cases on the Internet or try to look for images that we have not been able to locate due to low frequency. In addition, as this project has been done in English, it will provide the students with necessary tools to do a literature search, as most of the medical and dental literature is in English; thus far, providing the student with this material necessary to make the appropriate searched using keywords in English.

The magnetically-active, low-mass, triple system WDS 19312+3607 (Research Note)

Aims. We investigated in detail the system WDS 19312+3607, whose primary is an active M4.5Ve star previously inferred to be young (τ ~ 300–500 Ma) based on its high X-ray luminosity. Methods. We collected intermediate- and low-resolution optical spectra taken with 2 m-class telescopes, photometric data from the B to 8 μm bands, and data for eleven astrometric epochs with a time baseline of over 56 years for the two components in the system, G 125–15 and G 125–14. Results. We derived the M4.5V spectral types of both stars, confirmed their common proper motion, estimated their heliocentric distance and projected physical separation, determined their Galactocentric space velocities, and deduced a most-probable age of older than 600 Ma. We discovered that the primary, G 125–15, is an inflated, double-lined, spectroscopic binary with a short period of photometric variability of 1.6 d, which we associated with orbital synchronisation. The observed X-ray and Hα emissions, photometric variability, and abnormal radius and effective temperature of G 125–15 AB are indicative of strong magnetic activity, possibly because of the rapid rotation. In addition, the estimated projected physical separation between G 125–15 AB and G 125–14 of about 1200 AU ensures that WDS 19312+3607 is one of the widest systems with intermediate M-type primaries. Conclusions. G 125–15 AB is a nearby (d ≈ 26 pc), bright (J ≈ 9.6 mag), active spectroscopic binary with a single proper-motion companion of the same spectral type at a wide separation. They are thus ideal targets for specific follow-ups to investigate wide and close multiplicity or stellar expansion and surface cooling because of the lower convective efficiency.