  The primary goal of this study is to observe how complex the behaviors of
Cepheids can be, and to show how the continued monitoring of Cepheids at
multiple wavelengths can begin to reveal their "secret lives."
  We aim to achieve this through optical photometry, UV spectroscopy and X-ray
imaging. Through Villanova's guaranteed access to ground-based telescopes, we
have secured well-covered light curves as regularly as possible. Amplitudes and
times of max brightness were obtained and compared to previous literature
results. At UV wavelengths, we have secured hi-res spectra of 2 nearby Cepheids
- delta Cep and beta Dor - with HST-COS. Also, we have obtained X-ray images of
5 Cepheids with XMM-Newton and the Chandra X-ray Observatory, and further
observations with both satellites have been proposed for (XMM) and approved
(Chandra).
  Optical photometry has shown that 8 of the 10 observed Cepheids have
amplitude variability, or hints thereof, and all 10 show period variability
(recent, long-term or possibly periodic). The UV spectra reveal emission lines
from heated atmospheric plasmas of 10^4 - 10^5 K that vary in phase with the
Cepheid pulsations. The X-ray images have detected the three nearest Cepheids
observed (Polaris, delta Cep and beta Dor), while the distances of the other
two place their fluxes likely at or below detector background levels. The X-ray
fluxes for delta Cep show possible phased variability, but anti-correlated with
the UV emission lines (i.e. high X-ray flux during low UV flux, and vice
versa).
  Further data are required to ultimately confirm Blazhko-like cycles in
Cepheids, X-ray variability with phase and the particulars of the high-energy
variability such as phase-lags between atmospheric plasma emissions of
different temperature and the exact contributions of the possible heating
mechanism.
