0 Assigned ID: 3892 ----- Attempting Submission 1 (Fri Feb 17 19:50:45 GMT 2023) ----- INEFFICIENT ORDERING OF FP-POS POSITIONS Hi Amber, here's the repeat of the failed Visit 01. Cheers, Boris 600210456 ----- Attempting Submission 1 (Fri Mar 31 14:53:08 GMT 2023) ----- ----- Attempting Submission 2 (Tue Apr 04 15:04:36 GMT 2023) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 3 (Fri Oct 27 17:00:59 GMT 2023) ----- The warning regarding inefficient FP-POS switching can be ignored, as we switch back and forth between FP-POS=3 and 4 during Earth occultation. A detailed far-ultraviolet study of the planetary debris accreting onto the magnetic white dwarf Feige 7 Both photospheric metal pollution from the accretion of planetary debris, and strong (>MG) fields are, separately, detected among ~20% of all white dwarfs. However, the two features combined have so far only been observed in cool (<10000K) and old (>1Gyr) white dwarfs. The reason for this clustering is not well understood, but it may be related to how planet formation and the formation of magnetic fields depend on the white dwarf progenitor mass. We have identified Feige 7 as the first warm (~20000K) young (~200Myr) and strongly magnetic (~18MG) white dwarf that is actively accreting the debris of tidally disrupted planetesimals. The discovery of this system opens up the unprecedented opportunity to study atomic physics of C, Si, and potentially O, S, and Fe in an field that is orders of magnitude higher than what can be achieved in a laboratory on Earth. Modelling the Zeeman-split metal transitions, we will measure the photospheric abundances and infer the composition of the planetary debris. Comparison of these results with published composition studies will reveal if Feige 7 is distinct from the well-studied non-magnetic white dwarfs accreting planetary debris. Using spin-phase resolved spectroscopy, we will map both the magnetic field topology (from the Ly alpha Zeeman components) and the surface distribution of the accreted debris. This will represent the first detailed study of the accretion process, and inform our understanding of the lateral spreading of the planetary material accreted onto the white dwarf. The goal of these COS observations is to obtain phase-resolved COS/G130M FUV spectroscopy of the magnetic white dwarf Feige 77, fully sampling its spin period of 2.2h. The beat with the 96min HST orbit requires four consecutive orbits to achieve this goal. We split the observations into two visits, using each 1222A and 1291A as central wavelengths in one of them. Visit 1 (1291A) only uses FP-POS=3,4 because of the COS 2025 policy, which generates a warning message. Visit 2 (1222A) uses FP-POS=1,2,3,4. Apart from impacting the schedulability of this program, we do not foresee any negative effect should HST drop to a 2-gyro mode. This target (WDJ004345.98-100025.02 = Feige 7) was previously observed with COS/G130M as part of program 16642, the maximum flux level is ~1.5e-13erg/cm2/s/A. We use the same target acquisition as in the previous observation. https://archive.stsci.edu/cgi-bin/mastpreview?mission=hst&dataid=LEQC20010 Gaensicke has been PI of 20 HST programs, carrying out far-ultraviolet spectroscopy of white dwarfs, and will implement the observations, and lead the analysis. Landstreet is an expert in the modelling of the spectra of magnetic stars. Stopkowicz is a theoretical chemist with detailed expertise in the computational modelling of atomic physics in strong magnetic fields. Exoplanets and Exoplanet Formation Stellar Physics and Stellar Types 3 false false true false false false false false SUPPORTED STAR DB NO This target was previously observed with COS/G130M (exposure LEQC20010, https://archive.stsci.edu/cgi-bin/mastpreview?mission=hst&dataid=LEQC20010), the maximum flux level is ~1.5e-13erg/cm2/s/A. J2000 J2000 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 32.1. 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