11 orbits and cleared the special rrquirement-2086499380Assigned ID: 445
----- Attempting Submission 1 (Fri Apr 10 12:21:14 GMT 2015) -----
HST Phase I Proposal 445 (xi_per.apt) successfully submitted.
Receipt: # 445-1
----- Attempting Submission 2 (Fri Apr 10 19:25:30 GMT 2015) -----Nolan Walborn infomed me that my ACQ and ACQ/PEAK times were too long. So I've changed them and tweeked the E140M exposure times a little to fill up the orbits.328431410----- Attempting Submission 1 (Wed Jul 22 14:50:53 GMT 2015) -----
----- Attempting Submission 2 (Mon Aug 24 02:28:41 GMT 2015) -----The wind of ksi Per: a tomographic view of stellar wind dynamicsWe propose to obtain 11 STIS and 10 XMM spectra of ksi Per to provide the critical information needed to progress our understanding of the structure of O star winds. In recent years, it has become apparent that radiatively driven winds are far more complex than the homogeneous, spherically symmetric flows originally envisioned. Instead, they have been shown to contain optically thick structures which may be quite small or very large. Until we unravel the details of these structures and how they interact, we cannot hope to reliably translate observational diagnostics into physical quantities such as mass loss rates. The state of affairs is evident from the huge swings in the values of observationally derived mass loss rates that have appeared in the recent literature. The proposed set of combined HST and XMM observations are key to developing a coherent picture of wind flows, their structure and how they fit together. The proposed observations will provide conclusive proof of whether the discrete absorption components observed in UV wind line profiles are related to X-ray variability and they will provide the phase difference between the two, which determines their relative locations in the winds. Together with existing data, we will also explore the optical thickness and covering factor of the wind structures and use all of these data to begin to produce a comprehensive model of radiatively driven winds. These observations will guide theoretical progress for years to come. Further, the window of opportunity to obtain such an important and unique data set is closing.This proposal entails 11 HST orbits spaced roughly 10 hours apart to obtain 11 STIS E140M and 11 STIS G750M spectra. Exposure times were estimated using a mean of 30 IUE spectra of xi Per for the UV exposure times and an O7 star model reddened by E(B-V ) = 0.32 mag and normalized to V = 4:08 mag for the H alpha exposures.
These observations should occur near the middle of the XMM-Newton observing run (roughly 17 Feb, 2016) which spans a much longer time interval.HOT STARS12falsetruefalsefalse70SUPPORTEDSTARMAIN SEQUENCE OThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG750M6581Timing link suitability includes constraints ([02 After 01 by 0.3 to 0.3 days] [03 After 01 by 1.0 to 1.0 days] [05 After 01 by 2.0 to 2.0 days] [07 After 01 by 3.0 to 3.0 days] [09 After 01 by 4.0 to 4.0 days] [11 After 01 by 5.0 to 5.0 days])The scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.(Tic-Visit
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