We provide estimates of atmospheric pressure and surface composition on short-period rocky exoplanets with dayside magma pools and silicate vapor atmospheres. Atmospheric pressure tends toward vapor-pressure equilibrium with surface magma, and magma-surface composition is set by the competing effects of fractional vaporization and surface-interior exchange. We use basic models to show how surface-interior exchange is controlled by the planet's temperature, mass, and initial composition. We assume that mantle rock undergoes bulk melting to form the magma pool, and that winds flow radially away from the substellar point. With these assumptions, we find that: (1) atmosphere-interior exchange is fast when the planet's bulk-silicate FeO concentration is low, and slow when FeO concentration is high; (2) magma pools are compositionally well-mixed for substellar temperatures 2400 K, but compositionally variegated and rapidly variable for substellar temperatures 2400 K; (3) currents within the magma pool tend to cool the top of the solid mantle ("tectonic refrigeration"); (4) contrary to earlier work, many magma planets have time-variable surface compositions. Subject headings: planets and satellites: terrestrial planets -planets and satellites: physical evolution -planets and satellites: surfaces -planets and satellites: individual (Kepler-10 b, CoRoT-7 b, KIC 12557548 b, KOI-2700 b, K2-22 b, K2-19 d, WD 1145+017, 55 Cnc e, HD 219134 b, Kepler-36 b, Kepler-78 b, Kepler-93 b, WASP-47 e). arXiv:1606.06740v1 [astro-ph.EP] 21 Jun 2016 2. SETTING THE SCENE: CURRENTS VERSUS WINDS.Magma pool surface composition, X s , is regulated by magma currents ( §2.2), silicate-vapor winds ( §2.3), and the development of compositionally distinct surface zones ( §2.4). If currents transport much more mass than winds, then X s will be the same as pool-averaged composition X p . However, X s and X p may differ if winds outpace