Are the kinematical characteristics of the CNM at /b/ > 300 consistent with T he hypothesis of a local explosive event?

Details Are the kinematical characteristics of the CNM at /b/ > 300 consistent with T he hypothesis of a local explosive event? Are the kinematical characteristics of the CNM at /b/ > 300 consistent with T he hypothesis of a local explosive event?

Nov 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998larm.confe..62p&link_type=abstract

"IX Latin American Regional IAU Meeting, "Focal Points in Latin American Astronomy", held in Tonantzintla, Mexico, Nov 9-13, 199

Astronomy and Astrophysics

Astronomy

Scientific paper

In order to check this hypothesis (cf. Olano's models for Lindblad's ring, AA 112, 195,1982) we computed the positions and velocities of test particles, which were ejected isotropically from a point of coordinates l, b located at the distance r from the Sun. The computations were fitted to the observations of the cold neutral medium (CNM) derived in a former paper from HI-atlases (cf. AA 287, 601, 1994). The fit appears to be rather satisfactory for a large fraction of the observations. We point out that the test particles ejected toward the largest northern altitudes have no observational counterparts but fit roughly the well-known northern HI-hole. We suggest that this should be a signature of the explosion and indicates the ionization and transfer of gas into the lower halo. Among the regions presenting the largest disagreements with the fit are the large young Sco-Cen and Ori-Eri shells. We extended the models to include young disturbance centers producing radial accelerations on the test particles. As an application, the fit of the region of the Sco-Cen shells was significantly improved by assuming a disturbance center of coordinates, distance and age consistent with those of the Loop I. We conclude that the assumption of an explosive event about 35 Myr ago, al l =~ 1400, with r =~ 120 pc appears to be consistent with the observed kinematics of the CNM at /b/ > 300.

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