  HD3167b is a transiting super-Earth that has a density which is consistent
with a rocky composition. The planet is exposed to strong radiation, intense
stellar wind, and likely strong tidal forces and induction heating. According
to theory, planets that are so close to the star should have an atmosphere like
Mercury but much more extended and denser. Other theories predict that such
planets have a lava lake on their surfaces and exhibit an enormous volcanic
activity. We have calculated the heating by electromagnetic induction to
estimate if it can drive significant volcanic activity at HD3167b and shown
that for some magnetic fields the heating can be substantial. HD3167 is an
ideal target to search for the exosphere of a planet, and signs of volcanic
activity. We observed the planet in-and out-of transit with UVES in order to
search for presence of lines originating from the exosphere of the planet such
as the NaD1,2 and CaIIH&K lines as well as numerous [S II],[S III], and [O III]
lines that are tracers of volcanic activity. We derived upper limits for the
ratios of the line fluxes to the stellar flux. The upper limits that we derived
are Ip,lambda/I*,lambda=1.5 10-3 for the CaII,H&K lines, and
I_p,lambda/I*,lambda=7.2 10-4 and I_p,lambda/I_*,lambda=3.3 10-4 for the
NaD_1,2 lines, respectively. The fact that our upper limits correspond to
previous detections in 55 Cnc e shows that not all super-Earth show these lines
all the time and that they might be variable.
