  The magnetic field of the Solar corona is difficult to measure directly.
However, indirect observations of the solar corona are possible using the
deficit in flux of cosmic rays coming from the direction of the Sun. Low-energy
cosmic rays (~GeV) are deflected by the inner magnetic field of the Sun and the
interplanetary magnetic field frozen into the solar wind. In contrast,
high-energy cosmic rays (~TeV and above) are absorbed in the Sun's photosphere
producing a shadow in the Sun's nominal position viewed from Earth. Several
ground-based instruments have observed the effects of the heliospheric magnetic
field on the size of the sun shadow and its position. The High-Altitude Water
Cherenkov Observatory (HAWC) is an air shower array located in the central
region of Mexico that observes TeV cosmic rays at a rate of about 15 kHz. in
this work, we present preliminary images of the sun shadow from data collected
by HAWC during 2013 and 2014 for different energy ranges.
