  Type-I bursts (i.e. noise storms) are the earliest-known type of solar radio
emission at the metre wavelength. They are believed to be excited by
non-thermal energetic electrons accelerated in the corona. The underlying
dynamic process and exact emission mechanism still remain unresolved. Here,
with a combined analysis of extreme ultraviolet (EUV), radio and photospheric
magnetic field data of unprecedented quality recorded during a type-I storm on
30 July 2011, we identify a good correlation between the radio bursts and the
co-spatial EUV and magnetic activities. The EUV activities manifest themselves
as three major brightening stripes above a region adjacent to a compact
sunspot, while the magnetic field there presents multiple moving magnetic
features (MMFs) with persistent coalescence or cancelation and a
morphologically similar three-part distribution. We find that the type-I
intensities are correlated with those of the EUV emissions at various
wavelengths with a correlation coefficient of 0.7-0.8. In addition, in the
region between the brightening EUV stripes and the radio sources there appear
consistent dynamic motions with a series of bi-directional flows, suggesting
ongoing small-scale reconnection there. Mainly based on the induced connection
between the magnetic motion at the photosphere and the EUV and radio activities
in the corona, we suggest that the observed type-I noise storms and the EUV
brightening activities are the consequence of small-scale magnetic reconnection
driven by MMFs. This is in support of the original proposal made by Bentely et
al. (Solar Phys. 193, 227, 2000).
