Exploring the Role of Stellar Magnetic Fields in Accretion and Outflows from Young Stars using the Hot Emission Lines of Herbig Ae/Be Stars

I have changed some of the details of visit 04 after consultation with my instrument scientist. Specifically, I have changed the FUV MAMA exposures to a series of shorter ACCUM exposures. ----- Attempting Submission 3 (Fri Aug 24 04:39:48 GMT 2012) ----- ----- Attempting Submission 4 (Thu Aug 30 20:06:42 GMT 2012) ----- All of these have been run before on the original submission. I downloaded the version of this apt file from STScI and altered the exposure details of visit 4. Exploring the Role of Stellar Magnetic Fields in Accretion and Outflows from Young Stars using the Hot Emission Lines of Herbig Ae/Be Stars Most stars form surrounded by a circumstellar accretion disk. It is in these disks that planetary systems form. The ultimate fate of the material in these disks is determined by the competition between matter accreting onto the stellar surface, matter being launched into an outflow away from the star, and the formation of solar system like bodies. For low mass stars, strong stellar magnetic fields play key roles in the accretion and possibly outflow processes. While it is often assumed that stellar magnetic fields play a similarly important role for intermediate mass stars, the observational evidence for this is far from complete. This is due in part to a lack of detected accretion or outflow diagnostics in optical line profile studies which trace these mass flows. The limited existing UV data suggests that this may simply be the result of different temperatures in the flows for these two mass regimes; however, there is not enough data to know for certain. Here, we propose a small survey of a carefully selected sample of intermediate mass Herbig Ae/Be stars to determine the incidence of accretion and outflow signatures in their high temperature line profiles in order to establish whether these stars interact with their surrounding accretion disks in the same manner as their younger cousins. Our primary observational goal is to search for high-temperature wind and accretion signatures in HAEBE stars, which can be found in the UV. The target sample is composed of objects that do not show optical wind signatures (i.e. red-shifted absorptions) but present optical indicators of accretion as well as infrared excesses suggesting circumstellar disks. The spectral diagnostics that we will observe sample a variety of physical conditions. The main observational handles we use are the N V doublet (1240 A), the O I line (1302 A), the Si IV (1400 A) and C IV (1550 A) doublets and the He II (1640 A) line. Broad and strong emissions in C IV and He II are typical indicators of magnetospheric accretion in CTTSs. As the spectra of DX Cha suggests, C IV may also be a primary (hot) outflow diagnostic for HAEBES. O I presents a traditional P Cygni profile in CTTSs indicative of a cool wind (Herczeg et al. 2005, AJ, 129,2777). N V is a broad emission doublet in CTTS, indicative of accretion, partially absorbed by a N I outflow line. Other well known wind indicators (S III at 1527 A, C II at 1336 A) are also present in the spectral ranges sampled in these observations. In the FUV, COS is 10x faster than STIS. However, some targets are just above the safety limits for COS. Therefore, we design our observations as a mixture of COS-PSA and STIS-0.2x0.2. The exposure times are based on a visibility period (minus overhead) of 2200 sec. For the COS targets, each target will be observed for a total of two orbits with the spectral elements G130M, G160M, and G230L. The FUV gratings provide R ~ 22000 spectroscopy, which is enough to resolve P Cygni profiles in CTTSs and in DX Cha. The NUV grating (R ~ 3000) provides a simultaneous measurement of the accretion rate (Calvet & Gullbring 1998). The G130M observations at lambda_o=1291 A (exposure ~ 2200 sec) cover the spectral ranges 1132 -1274 A and 1291 -1433 A. For the faintest target in the sample, the expected continuum S/N ~ 12 at 1250 A. Analogously, the G160M observations at lambda_o=1577 A (exposure ~ 2000 sec) cover the spectral ranges 1382 - 1556 A and 1577 - 1752 A. For the faintest target in the sample, the expected continuum S/N ~ 13 at 1550 A. The G230L are done at lambda_o=2950 A (exposure ~ 200 sec), measuring the spectral ranges from 1650-2050 A and 2750-3150 A. The continuum S/N ~ 30 at 2800 A. For the STIS targets, each target will be observed with E140M (1144 -1729 A and R ~ 90000) for almost two orbits, reaching a S/N comparable to that of COS. Each target will also be observed with STIS G230L (0.2x0.2) for 200 sec to measure the accretion rate. The total orbit request comes to 20 orbits. STAR FORMATION 12 false 0.0 0.0 false false false false SUPPORTED STAR A0-A3 V-IV HERBIG AE/BE J2000 J2000 STAR HERBIG AE/BE J2000 J2000 STAR HERBIG AE/BE J2000 J2000 STAR HERBIG AE/BE J2000 J2000 STAR HERBIG AE/BE J2000 J2000 STAR HERBIG AE/BE J2000 J2000 STAR HERBIG AE/BE J2000 J2000 STAR HERBIG AE/BE J2000 J2000 STAR HERBIG AE/BE J2000 J2000 STAR HERBIG AE/BE J2000 J2000 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No E140M 1425 COS/NUV Spectroscopic No No G230L 2950 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1291 COS/NUV Spectroscopic No No G230L 2950 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1291 COS/NUV Spectroscopic No No G230L 2950 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1291 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No E140M 1425 COS/NUV Spectroscopic No No G230L 2950 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1291 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No E140M 1425 COS/NUV Spectroscopic No No G230L 2950 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G130M 1291 The scheduling data was generated by CASM 20.2. CASM was run in Phase II mode. 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