  Magnetic elements of the solar surface are studied in magnetograms recorded
with the high-resolution Solar Dynamics Observatory / Helioseismic and Magnetic
Imager . To extract some statistical and physical properties of these elements
(e.g., filling factors, magnetic flux, size, lifetimes), the Yet Another
Feature Tracking Algorithm (YAFTA), a region-based method, is employed. An area
with 400$^{\prime\prime}\times$400$^{\prime\prime}$ was selected to investigate
the magnetic characteristics during the year 2011. The correlation coefficient
between filling factors of negative and positive polarities is 0.51. A broken
power law fit was applied to the frequency distribution of size and flux.
Exponents of the power-law distributions for sizes smaller and greater than 16
arcsec$^2$ were found to be -2.24 and -4.04, respectively. The exponents of
power$-$law distributions for fluxes smaller and greater than
2.63$\times$10$^{19}$ Mx were found to be -2.11 and -2.51, respectively. The
relationship between the size ($S$) and flux ($F$) of elements can be expressed
by a power-law behavior in the form of $S\propto F~^{0.69}$. The lifetime and
its relationship with the flux and size of quiet-Sun (QS) elements are studied
during three days. The code detected patches with lifetimes of about 15 hours,
which we call long-duration events. It is found that more than 95\% of the
magnetic elements have lifetimes of less than 100 minutes. About 0.05\% of the
elements were found with lifetimes of more than 6 hours. The relationships
between the size (S), lifetime (T), and the flux (F) for patches in the QS,
indicate the power$-$law relationships $S\propto T~^{0.25}$ and $F\propto
T~^{0.38}$, respectively. Executing a detrended fluctuation analysis of the
time series of new emerged magnetic elements, we find a Hurst exponent of 0.82,
which implies long-range temporal correlation in the system.
