  Context. A region at the inner edge of the main asteroid belt is populated by
the Hungaria asteroids. Among these objects, the Hungaria family is formed as
the result of a catastrophic disruption of (434) Hungaria asteroid hundred
million years ago. Due to the Yarkovsky effect, the fragments depending on
their direction of rotation are slowly drifting inward or outward from the
actual place of collision. Due to this slow drift these bodies could approach
the locations of the various mean-motion resonances (MMRs) of outer type with
Mars. Aims. We aim to study the actual dynamical structure of Hungaria
asteroids that is primarily shaped by various MMRs of outer type with Mars.
Moreover, we also seek connections between the orbital characteristics of
Hungaria asteroids and their absolute magnitude. Methods. To map the resonant
structure and dynamics of asteroids belonging to the Hungaria group, we use the
method FAIR (as FAst Identification of mean motion Resonances), which can
detect MMRs without the a priori knowledge of the critical argument. We also
compile stability maps of the regions around the MMRs by using the maximal
variations in the asteroids' eccentricities, semi-major axes, and inclinations.
We numerically integrate the orbits of all asteroids belonging to the Hungaria
group available in the JPL Horizon database together with the Solar System
planets for one and ten million years. Results. Having studied the resonant
structure of the Hungaria group, we find that several asteroids are involved in
various MMRs with Mars. We identify both short and long-term MMRs. Besides, we
also find a relationship between the absolute magnitude of asteroids and the
MMR in which they are involved.
