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	In combination with space and ground-based observations, H-alpha
		full disk observations of high temporal and spatial resolution
		have been proven to be a key diagnostic for determining the
		magnetic field topology between the photosphere, chromosphere,
		transition region, and corona.
	Continuous H-alpha network observations will ensure the 
		tracking of features near the poles continuously. By
		this the accuracy of solar rotation rate measurements
		will be increased.
	Studying prominences and corresponding filaments simultaneously
		provides deeper insight into their temporal evolution and their
		supporting magnetic field configuration.
	Flares can occur anywhere and at any time on the solar disk.
		High resolution solar images with 24 hour coverage are essential
		to catch all the flares on the visible disk of the Sun.
	High spatial resolution and cadence will allow to obtain a detailed
		picture of the evolution of flares as well as of the associated
		active regions.
	Until now, H-alpha full disk images depicting solar flares were
		normally saturated because the exposure time was set to a
		constant value and optimized to yield high contrast images of 
		the quiet Sun. The bright flaring regions were therefore
		over-exposed. Since the H-alpha intensity gives a minimum
		temperature for the flare region, it is important to obtain
		proper photometric data even when the full disk brightness
		is suddenly rising during a flare.
	Monitoring every new flux emergence and try to understand why
		some become super-active regions and other decay quickly.
	Providing high quality data for solar activity forecasting.
	Providing complete data sets for correlative studies with other
		ground-based and space observations.
	Observing and classifying all the flares and filament/prominence
		eruptions obtained by the network.
	One of the ongoing research projects at BBSO is to understand
		the correlation between filament/prominence disappearance and
		coronal mass ejections (CMEs) and to study their possible
		driving mechanisms. Round-the-clock high-resolution full disk
		H-alpha data are extremely important for this study, as CMEs
		may occur anywhere and at any time on the Sun.
	Mini-filament eruptions are the small scale analog to large scale
		filament eruptions. The energy release and mass ejection of 
		erupting mini-filaments is of particular importance since
		both can contribute to coronal heating and solar wind
		acceleration. With high contrast and high cadence H-alpha
		images the position and therefore the spatial distribution
		of mini-filaments as well as their temporal behavious is easy 
		to measure.
	Round-the-clock high-resolution H-alpha observations will be able
		to provide data with sufficient resolution and cadence to
		support the observing targets of space observations, anywhere
		on the face of the Sun and at any time.
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