0 Submission failed communicating with the submission server: java.rmi.ConnectException: Connection refused to host: 130.167.201.116; nested exception is: java.net.ConnectException: Connection timed out: connect Submission failed communicating with the submission server: java.rmi.UnknownHostException: Unknown host: clotho.stsci.edu; nested exception is: java.net.UnknownHostException: clotho.stsci.edu Assigned ID: 766 ----- Attempting Submission 1 (Fri Feb 24 21:53:09 GMT 2012) ----- HST Phase I Proposal 766 (HST Cycle 20 Cepheids.apt) successfully submitted. ----- Attempting Submission 2 (Fri Feb 24 22:08:16 GMT 2012) ----- Retained the Phase requirement for the first exposure of visit 01, but removed it from subsequent exposures during this visit, to prevent any software confusion. 1520433498 ----- Attempting Submission 1 (Tue Jul 10 16:53:03 GMT 2012) ----- HST Phase II Proposal 13019 (HST_Cycle20_Cepheids.apt) successfully submitted. ----- Attempting Submission 2 (Fri Sep 28 20:33:20 GMT 2012) ----- HST Phase II Proposal 13019 (HST_Cycle20_Cepheids.apt) successfully submitted. ----- Attempting Submission 3 (Thu Oct 11 19:37:44 GMT 2012) ----- ----- Attempting Submission 4 (Wed Feb 20 19:14:54 GMT 2013) ----- ----- Attempting Submission 5 (Tue Jun 11 19:46:38 GMT 2013) ----- HST Phase II Proposal 13019 (HST_Cycle20_Cepheids_II.apt) successfully submitted. ----- Attempting Submission 6 (Fri Jun 14 17:02:40 GMT 2013) ----- All warnings have been noted. If further clarification is necessary, just let us know. scott.engle@villanova.edu edward.guinan@villanova.edu Probing the Complicated Atmospheres of Cepheids with HST-COS: Plasma Dynamics, Shock Energetics and Heating Mechanisms Classical Cepheids, although well studied in terms of their cosmologically important Period-Luminosity Law, are proving to be increasingly complex and astrophysically intriguing in terms of the atmospheric energetics. This proposal expands Cycle 17/18 programs to probe Cepheid atmospheres and understand the mechanisms by which they are heated. Our previous COS spectra revealed a wealth of 10,000-300,000K plasma emission lines (far beyond what previous IUE data show due to severe scattered light contamination), phase-locked with the Cepheid pulsation periods, indicating that a pulsation-driven heating mechanism is at work. We propose multiple observations of selected Cepheids (delta Cep, beta Dor and l Car) with HST-COS through the G130M & G160M gratings, to provide comprehensive and detailed diagnostics of the atmospheric plasmas of Cepheids with a range of periods and pulsation types, and give the best look yet at how large-scale, radial pulsations affect the upper atmospheres of supergiants. The phase constraints placed on some of the visits will allow phase-lags between the emission lines to be detailed, giving important additional information on the heating mechanism and extents of the atmospheres. Numerous emission lines are covered by the G130M and G160M wavelength range (~1150-1750A), including N V 1240, O I, C IV 1550 and He II 1640. When combined with our approved and future proposed X-ray observations of Cepheids, the HST-COS data will allow us to construct an understanding of Cepheid atmospheric plasmas with temperatures of tens of thousands to millions of degrees -- the most thorough atmospheric study to date for this important class of pulsating stars. We propose 9 HST-COS visits (1 orbit each) of 3 selected Cepheids (in the HST continuous viewing zone) to: finish work we have begun on |*| Cep and |*| Dor in Cycles 17 and 18; and expand our COS Cepheid database to include the long period l Car. We propose phase-constrained observations near |*| = 0.93 for |*| Cep and near |*| = 0.64 and 0.72 for |*| Dor, thus helping complete the phase coverage (leading to a much better understanding of what we believe to be shock propagation through the stellar atmosphere). The |*| Cep observation will occur at a very important phase just after the large-scale atmospheric infall (where a second shock could easily be initiated), and help us determine specific phase peaks of different emission species, along with line ratios and flow velocities. For |*| Dor, although our Cycle 18 observations had a good phase spread, this Cepheid shows a large phase-lag between different emission species. As a result, only the peak of N V is characterized, with all other emission lines caught sometime after maximum, preventing the true scale of their variability from being recorded. The two requested Cycle 20 observations will allow us to compare the variabilities of all emission lines in |*| Dor, along with their flow velocities. We propose 6 visits on l Car to cover the maximum emission phases we expect, based on data thus far. l Car is a very exciting target for several reasons: as by far the longest period Cepheid in this program (~35.5-day period), it is markedly different from the other targets, shows full-amplitude light and RV variability, and archival IUE data show it to have the strongest emissions of all observed Cepheids. In fact, the IUE data have also shown periodic UV variability, but the scattered light (again) overwhelmed all but the absolute strongest lines from appearing. l Car is also much larger than our other program Cepheids (~180R|*| according to Taylor et al. 1997; where |*| Dor is the next largest in the program at ~75R|*|), and the same study also found two possible shocks along the RV curve at |*| = 0.7, 0.9. The phase-constrained visits we request for l Car will occur at and around these phases. Finally, l Car is of later spectral type and will have less photospheric continuum obscuring some of the longer-wavelength lines in this study. COOL STARS 12 false false 0.0 0.0 false false false SUPPORTED STAR CEPHEID G III-I This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR CEPHEID G III-I This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STAR CEPHEID G III-I This object was generated by the targetselector and retrieved from the SIMBAD database. 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