A X-ray through Radio Exo-Space Weather Campaign to Study the Young Sun, EK Dra

sub 2, 11/14/23, 16:24 MST. kevin.france@colorado.edu -2047582102 Assigned ID: 4908 ----- Attempting Submission 1 (Tue Nov 14 23:25:12 GMT 2023) ----- HST Phase I Proposal 4908 successfully submitted. Receipt: # 4908-1 ----- Attempting Submission 2 (Wed Nov 15 00:32:31 GMT 2023) ----- HST Phase I Proposal 4908 successfully submitted. Receipt: # 4908-2 INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS We would like to request that these observations be scheduled durng Japanese nighttime hours (10-20 UTC) to facilitte the multi-wavelength coordination for this observing program. Moved to proper motion epoch 2000 following discussions with the contact scientist. 02/01/24 Thank you! Kevin France -2102290321 ----- Attempting Submission 1 (Thu Jan 25 12:43:03 GMT 2024) ----- HST Phase II Proposal 17595 successfully submitted. Receipt: # 17595-1 ----- Attempting Submission 2 (Thu Feb 01 20:00:30 GMT 2024) ----- A X-ray through Radio Exo-Space Weather Campaign to Study the Young Sun, EK Dra The focus of the proposed study is the magnetic activity of the young (50 -125 Myr) Sun-like star, EK Draconis. This nearby star thought to be an ideal proxy of the infant Sun at a near-zero-age main-sequence epoch, when the Earth's atmosphere transitioned from the primary to the secondary nitrogen and carbon dioxide rich atmosphere. Thus, the knowledge of the stellar ionizing radiation in the form of quiescent and flare X-ray and EUV emission, stellar wind and CME pressure that can affect the atmospheric escape and its chemistry is of critical importance for the study of early Venus, Earth and Mars environments. EK Dra is the subject of a recently-approved multi-wavelength ground- and space-based observing campaign and we propose to obtain new HST far-UV (FUV) spectra and light curves and combine these with scheduled optical spectropolarimetry (SEIMEI), TESS, and NICER X-ray observations, while radio (GMRT) radio observations of EK Dra have been proposed. Most importantly, the contemporaneous nature of these observations will provide a physically consistent picture of the drivers and outputs of the magnetically driven stellar coronal and wind structures of infant suns. We will use these observations as inputs to a fully thermodynamic model of the corona-wind system of EK Dra using the AWSoM code. AWSoM will output the missing EUV and stellar wind parameters that are required to predict the atmospheric evolution of terrestrial planets orbiting young suns. FUV Spectra: The HST data will use COS with G130M, CENWAVE=1309 to record the emission lines of C III (117.5 nm), Si III (120.6 nm), N V (123.8nm), Fe XII (124.2, 134.9nm), C I (132.9nm), C II (133.5 nm), Fe XXI (135.4nm), O V (137.1nm), O IV] (140.1nm), and Si IV (139.4, 140.3 nm). To resolve the physical processes relevant to chromospheric and coronal heating, we require R ~ 15,000. To constrain the stellar wind density of EK Dra, we require signal-to-noise ~ 10 at the peak of the O IV] 140.1 nm line. By comparing to archival HST FUV spectra of EK Dra (Ayres & France 2010; Ayres 2015), we estimate that three orbits per visit will be sufficient for detection of S/N > 10 per resolution element in the peak of the density-sensitive O IV] features (COS.sp.1684389). We calculate S/N between 10 and 20 in the peak of several C I lines and the coronal iron lines, S/N between 20 and 30 in Si IV and N V, and S/N > 30 in Si III and C II. This highfidelity spectrum will allow us to identify temporal variability and will provide robust line-fit measurements of thermal and non-thermal widths and line kinematics. Given the observed UV flare rate from EK Dra, we expect to observe 2 - 3 multi-wavelength flares in a 12 orbit HST campaign (3 orbits per visits x 4 visits). Each 3-orbit visit is sufficient for a high-S/N stellar spectrum (see next sub-section) that will provide the quiescent stellar baseline and rotational modulation between flare events. Target Acquisition: We performed a quantitative ETC target acquisition calculation using the STScI online tools, we scaled observed solar-type star to an average magnitude of V = 7.6, and we find that an exposure time of approximately 3.2s are required (COS.ta.1684394), using an imaging target acquisition in BOA+MIRRORA. Instrument Safety: An ETC calculation using the observed EK Dra Lyman-alpha flux (the brightest stellar line in the FUV spectrum of EK Dra; Ayres et al. 2015), multiplied by 1.5 for conservatism, find no bright object violations using the COS G130M mode (COS.sp.1895208), therefore these observations present no risk to the instrument and are consistent with the COS 2025 observing guidelines. Coordinated Observations: Simultaneous observations from space- and ground-based telescopes using X-ray spectroscopy (NICER), optical spectroscopy/photometry (TESS, Seimei telescope), and radio telescope (GMRT) will complement the HST time. TESS will be pivotal for the calculation of global energies. These observatories have a long record of providing flexible scheduling to provide supporting ground-based observations for approved space-based flare campaigns. PI: K. France - University of Colorado Kevin France is the PI of the HST MUSCLES Treasury Survey (GO13650) and MEATS (GO16166) Survey to study the spectral and temporal properties of exoplanet host stars (France et al. 2016, 2018, 2020; Loyd et al. 2016; Youngblood et al. 2016). He is the co-PI of the follow-on Mega-MUSCLES (GO15071) and Mega-MEATS (16701) Surveys that focused on activity in stars optimal for planetary characterization with JWST. He was a member of the COS instrument and science teams; he is intimately familiar with HST-COS and -STIS instrument, data, and analysis procedures. His research group has developed numerous community tools for spectral and temporal analysis of COS and STIS data. Dr France has authored over 70 refereed publications on exoplanets, cool stars, and planet-forming disks using UV spectra from HST. Vladimir Airapetian is Senior Astrophysicist at Heliophysics Science Division, NASA Goddard Space Flight Center and Research Professor at American University, DC. He is an internationally known expert in theoretical modeling of the Sun and young solar analogs including solar-stellar magnetic fields, flare physics, and impacts on planetary atmospheres. He leads several NASA projects relating to exoplanet habitability and astrobiology. He is responsible for MHD modeling of the corona-wind system as well as flare and CMEs from EK Dra. Kosuke Namekata is an expert in multi-wavelength observations of G-dwarf stellar flares, from the X-ray to the optical. He has extensive experience and publications on observations and analysis using the Seimei telescope, TESS, and NICER. Stellar Physics and Stellar Types Exoplanets and Exoplanet Formation 0 false false true false false true false false SUPPORTED EXT-STAR G V-IV NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 COS/FUV Spectroscopic No No G130M 1291 1706814949281 C:\DDRIVE\GTO2008\GO_Cy31\OP-cache\EKDRA_mid31_ph2_v2-v01.xml Timing link suitability includes constraints ([02 After 01 by 0.5 to 2.0 days]) The scheduling data was generated by CASM 32.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17595 :visit-id "01" :proposal-version -1 :trans-version "20230626" :date "01-Feb-2024 12:15:48.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 495824 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17595 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17595 :visit-id "01" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2499 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17595 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17595 :visit-id "01" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 436 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) true 3 0 1706814950174 C:\DDRIVE\GTO2008\GO_Cy31\OP-cache\EKDRA_mid31_ph2_v2-v02.xml Timing link suitability includes constraints ([02 After 01 by 0.5 to 2.0 days] [03 After 02 by 0.5 to 2.0 days]) The scheduling data was generated by CASM 32.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17595 :visit-id "02" :proposal-version -1 :trans-version "20230626" :date "01-Feb-2024 12:15:49.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 495824 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17595 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17595 :visit-id "02" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2499 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17595 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17595 :visit-id "02" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 436 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) true 3 0 1706814950968 C:\DDRIVE\GTO2008\GO_Cy31\OP-cache\EKDRA_mid31_ph2_v2-v03.xml Timing link suitability includes constraints ([03 After 02 by 0.5 to 2.0 days] [04 After 03 by 0.5 to 2.0 days]) The scheduling data was generated by CASM 32.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17595 :visit-id "03" :proposal-version -1 :trans-version "20230626" :date "01-Feb-2024 12:15:50.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 495824 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17595 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17595 :visit-id "03" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2499 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17595 :visit-id "03" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17595 :visit-id "03" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 436 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) true 3 0 1706814951870 C:\DDRIVE\GTO2008\GO_Cy31\OP-cache\EKDRA_mid31_ph2_v2-v04.xml Timing link suitability includes constraints ([04 After 03 by 0.5 to 2.0 days]) The scheduling data was generated by CASM 32.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 17595 :visit-id "04" :proposal-version -1 :trans-version "20230626" :date "01-Feb-2024 12:15:51.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 495824 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17595 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17595 :visit-id "04" :orbit-number 1 :pcs-time 443 :si-vis-utilization 2499 :al-overhead-at-end 0 :internal-dur-at-end 105 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17595 :visit-id "04" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17595 :visit-id "04" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2550 :al-overhead-at-end 0 :internal-dur-at-end 436 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2942 :pcs-gap 0 ) true 3 0