  The eruption of a large quiescent prominence on 17 August 2013 and associated
coronal mass ejection (CME) were observed from different vantage points by
Solar Dynamics Observatory (SDO), Solar-Terrestrial Relations Observatory
(STEREO), and Solar and Heliospheric Observatory (SOHO). Screening of the quiet
Sun by the prominence produced an isolated negative microwave burst. We
estimated parameters of the erupting prominence from a model of radio
absorption and measured from 304 \AA\ images. Their variations obtained by both
methods are similar and agree within a factor of two. The CME development was
studied from the kinematics of the front and different components of the core
and their structural changes. The results are verified using movies in which
the CME expansion was compensated according to the measured kinematics. We
found that the CME mass ($3.6 \times 10^{15}$ g) was mainly supplied by the
prominence ($\approx 6 \times 10^{15}$ g), while a considerable part drained
back. The mass of the coronal-temperature component did not exceed $10^{15}$ g.
The CME was initiated by the erupting prominence, which constituted its core
and remained active. The structural and kinematical changes started in the core
and propagated outward. The CME structures continued to form during expansion,
which did not become self-similar up to $25 R_\odot$. The aerodynamic drag was
insignificant. The core formed until $4 R_\odot$. Some of its components were
observed to straighten and stretch forward, indicating the transformation of
tangled structures of the core into a simpler flux rope, which grew and filled
the cavity as the CME expanded.
