  In this work we present data from observations with the MAGIC telescopes of
SN 2014J detected in January 21 2014, the closest Type Ia supernova since
Imaging Air Cherenkov Telescopes started to operate. We probe the possibility
of very-high-energy (VHE; $E\geq100$ GeV) gamma rays produced in the early
stages of Type Ia supernova explosions. We performed follow-up observations
after this supernova explosion for 5 days, between January 27 and February 2 in
2014. We search for gamma-ray signal in the energy range between 100 GeV and
several TeV from the location of SN 2014J using data from a total of $\sim5.5$
hours of observations. Prospects for observing gamma-rays of hadronic origin
from SN 2014J in the near future are also being addressed. No significant
excess was detected from the direction of SN 2014J. Upper limits at 95$\%$
confidence level on the integral flux, assuming a power-law spectrum,
d$F/$d$E\propto E^{-\Gamma}$, with a spectral index of $\Gamma=2.6$, for
energies higher than 300 GeV and 700 GeV, are established at
$1.3\times10^{-12}$ and $4.1\times10^{-13}$ photons~cm$^{-2}$s$^{-1}$,
respectively. For the first time, upper limits on the VHE emission of a Type Ia
supernova are established. The energy fraction isotropically emitted into TeV
gamma rays during the first $\sim10$ days after the supernova explosion for
energies greater than 300 GeV is limited to $10^{-6}$ of the total available
energy budget ($\sim 10^{51}$ erg). Within the assumed theoretical scenario,
the MAGIC upper limits on the VHE emission suggest that SN 2014J will not be
detectable in the future by any current or planned generation of Imaging
Atmospheric Cherenkov Telescopes.
