The unique ID for this investigator matches Dr. Cecilia Garraffo in the STScI database. Dear Shelly, here is the Cycle 24 installment of this program, it's very much the same as in Cycle 22 & 23 - we don't have the window for the XMM observations yet, so the visit is on hold. Boris -1453339193 Your proposal could not be saved. Submission aborted. ----- Attempting Submission 1 (Fri Jul 22 08:06:10 GMT 2016) ----- Looks like one of the CoIs is not in the STScI data base. The period distribution of close binaries, cataclysmic variables, novae and single-degenerate SN1a progenitor candidates is largely controlled by magnetically-driven mass and angular momentum loss (AML) from the M dwarf secondary. The mass loss rates for these spun-up stars remain essentially unknown and impossible to observe directly, with likely values in the range 1e-12 to 1e-15 Msun/yr. AML presciptions for CVs differ by orders of magnitude. One way to measure the mass loss rate is to observe the dM wind accrete onto its WD companion in a pre-CV very close to Roche Lobe overflow but lacking the obscuring complications and emission from an accretion disk. The measurement can be combined with realistic MHD models to understand the accretion fraction, the mass that escapes, and the AML. The best-studied nearby pre-CV is QS Vir (48pc, P=3.6hr). However, its wind accretion rates measured from 1999 HST UV spectra of the WD metal absorption lines and 2006 XMM-Newton CCD spectroscopy differ by a factor of a thousand, pointing to either a dominant CME stochastic component, or a "magnetic switch" found in MHD simulations and driven by cyclic activity on the M dwarf. HST COS spectra combined with XMM-Newton monitoring on timescales from weeks to years will tease out CME vs cyclic accretion variations. UV and X-ray measurements will provide the first consistency check of both accretion rate measurement methods. MHD models tailored to the system will enable the first quasi-direct measurements of the mass loss and AML from a CV-like binary. Our project requires 6 HST/COS orbits in Cycles 22-24, and 60ksec on XMM in Cycle 22 The target of this proposal is QS Vir, a well-studied detached white dwarf plus M-dwarf binary with an orbital period of 3.61h. The aim of this program is to provide measurements of the wind loss rate of an M-dwarf by measuring (quasi)simultaneously the X-ray luminosity generated by the accretion of the wind onto the white dwarf, and the photospheric abundances of the metals ingested into the atmosphere of the white dwarf. We don't have a date of the XMM observations, so the HST visit is put "on hold" One additional complication is that QS Vir is eclipsing, and the COS target acquisition has to avoid the eclipse of the white dwarf, as there is no UV flux left to acquire on. COOL STARS 6 false true false false false 60 false AVAILABLE STAR COMPOSITE SPECTRAL TYPE DA M V-IV NO QS Vir is a detached WD + M-dwarf binary, which has been previously observed with HST/STIS in the FUV and NUV (O57E51010, O57E51020, O57EB1010, O57EB1020), and has a well-defined ultraviolet, flux, F(1300A)=4.5e-14erg/cm2/s/A J2000 J2000 F(1300A)=4.5e-14erg/cm2/s/A COS/FUV Spectroscopic No No G140L 1105 1499780655578 Phase windows are not calculated when the gap between schedulable intervals is less than 1 days, assuming no scheduling restrictions for constraint Phase 0.200/0.800. The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. /private/var/folders/q_/glfmvhmj0mq4qm_yvhs134lh0003lp/T/OPVisit6714615703589857540.xml This visit should be scheduled as close as possible to the XMM observations of QS Vir. We will provide the exact data of the XMM observations as soon as we get to know from the XMM operations team. The target acquisition has to avoid the eclipse of the WD, as there is not sufficient UV flux left during the eclipse. (Tic-Visit :proposal-id 14702 :visit-id "01" :proposal-version -1 :trans-version "20170613" :date "11-Jul-2017 09:44:15.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 417600 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14702 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14702 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2895 :al-overhead-at-end 0 :internal-dur-at-end 350 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3209 :pcs-gap 0 ) false 1 1 On hold until we know the window of the XMM observations