! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5870,v 6.1 1995/06/28 23:57:03 pepsa Exp $ ! ! Refer to the HST Phase II Proposal Instructions to fill this out ! ! Anything after a "!" is ignored, and may be deleted ! ! All keywords with multiple entries are comma delimited except the ! Visit_Requirements and Special_Requirements keywords which can be ! delimited with carriage returns or semi-colons, but not commas ! ! For help call your Program Coordinator: Karla Peterson ! Phone: 410 338-4774, E-mail: peterson@stsci.edu ! ! This partially completed template was generated from your Phase I proposal. ! Proposal_Information ! Section 4 Title: Dead Or Just Sleeping? Status of Magnetic Dynamos in ``Maunder Minumum" Stars Proposal_Category: GO Scientific_Category: Cool Stars Cycle: 5 Investigators PI_name: Dr. Steven Saar PI_Institution: Smithsonian Astrophysical Observatory CoI_Name: Dr. Sallie Baliunas CoI_Institution: Smithsonian Astrophysical Observatory Contact: N ! Y or N (designate at most one contact) CoI_Name: Dr. Robert Donahue CoI_Institution: Smithsonian Astrophysical Observatory Contact: N ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) The Maunder minimum (and similar episodes occurring every few centuries) is a poorly understood 75 year period in which the normal solar magnetic dynamo cycle was temporarily interrupted. Its study is important for understanding the generation and evolution of solar/stellar magnetic fields, and for the possible influence of magnetic flux on the Sun's luminosity and hence on earth's climate. We propose to study the Maunder mimimum state by obtaining HRS spectra of a sample of solar-like stars which appear to be in the stellar analog of the Maunder minimum: i.e., stars with weak, nonvariable Ca II emission and long periods of rotation. Using transition region line emission as a proxy for magnetic fields, we will determine the residual magnetic activity levels of Maunder stars, the magnetic contribution to the total energy budget of their outer atmospheres, and explore the relations between Maunder activity levels and stellar mass and rotation. Only HST has the sensitivity to detect or usefully constrain the very weak emission seen in these stars. The results will be used to explore the evolution of dynamos with time, define the dependence of Maunder minimum activity on mass and rotation rate, test non-linear dynamo models, and estimate what solar conditions are like during a Maunder episode. Questions ! Free format text (please update) Observing_Description: We propose to take deep, far UV HRS spectra of all known late F, G and early K dwarfs which appear to be in a ``Maunder minimum-like" state: i.e., stars which are old (large P_ rot, low Li I abundance) and show weak, non- variable Ca II H+K emission. These spectra will be used to search for signs of high temperature T >= 10^5 K plasma, such as emission in Si IV (1400 Angstrom) and C IV (1550 Angstrom). Presence of these lines will indicate the existence of magnetic fields. Comaprison of their ratios to cooler chromospheric lines (e.g., C II 1335 Angstrom, O I 1305 Angstrom) relative to ratios seen in ``normal" cool stars will imply the fractional contribution of magnetic heating to the energy balance in the outer atmosphere. To obtain the necessary lines at adequate resolution, we will use the HRS with the G140L grating (LSA). This combination is much more sensitive than the FOS + G130H shortward of C IV and has a much lower scattered light. We can estimate the exposure time needed by scaling from the C IV flux of a MM star detected with IUE (HD 10700). This star has f_C IV = 5 * 10^-14 ergs cm^-2 s^-1 AA^-1, equivalent to a surface flux of F_C IV ~ 0.5 F_C IV(\odot). Few stars will be much older than HD 10700 (it is an old disk subdwarf), but we would like to be able to make 4 Sigma detections of C IV in stars with 5 times less surface flux - this would allow for a range of possible MM F_C IV values as a function of mass or age. (We relax this constraint to a 3 Sigma detection for our three faintest targets.) This exposure level also allows stringent limits to be placed on the existence of stars in the sample with no magnetic dynamos operating, and allows detection of fainter lines at somewhat lower significance (e.g., Si IV at ~ 2.5 Sigma). With an efficiency of 67* 10^11 counts s^-1 diode^-1 per incident erg cm^-2 s^-1 at C IV, HD 10700 would require an t_ exp ~ 2 minutes to obtain the required S/N. Values for the other stars were scaled from this value, including corrections for dark counts in the fainter stars (Table 1). Note that due to the length of the HST orbit, we will typically observe each star longer than the minimum t_ exp given in Table 1, yielding even more accurate detections or lower limits to the line fluxes. Real_Time_Justification: None. We will attempt contemporaneous observations of our target stars in Ca II H+K emission flux from Mt. Wilson observatory and otehr chromospheric diagnostics (e.g., H-Alpha, He I D3) from Kitt Peak. Ongoing time-flexible observational programs at both sites will make this plan easy to schedule. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: HD3651 Alternate_Names: GSC1193-02068, 54-PSC Description: STAR,K V-IV Position: RA = 00H 39M 21.72S +/- 0.01S, DEC = 21D 15' 2.1" +/- 0.1", Equinox: J2000 RV_or_Z: V=-34 RA_PM: -0.0331 Dec_PM: -0.366 Epoch: 2000.000 Annual_Parallax: 0.095 +/- 0.005 Flux: V=5.86 +/- 0.02 B-V=0.85 +/- 0.02 Comments: Coordinates are from Hipparcos INCA Target_Number: 2 Target_Name: HD9562 Alternate_Names: GSC4687-02318 Description: STAR,G V-IV Position: RA = 01H 33M 42.85S +/- 0.01S, DEC = -07D 01' 31.4" +/- 0.1", Equinox: J2000 RV_or_Z: V=-15 RA_PM: 0.0118 Dec_PM: -0.077 Epoch: 2000.000 Annual_Parallax: 0.095 +/- 0.005 Flux: V=5.74 +/- 0.02 B-V=0.64 +/- 0.02 Comments: Coordinates are from Hipparcos INCA Target_Number: 3 Target_Name: HD29645 Alternate_Names: GSC2893-02218 Description: STAR,G V-IV Position: RA = 04H 41M 50.26S +/- 0.01S, DEC = 38D 16' 48.8" +/- 0.1", Equinox: J2000 RV_or_Z: V=47 RA_PM: 0.0201 ! need improvement Dec_PM: -0.096 ! need improvement Epoch: 2000.000 Annual_Parallax: 0.022 +/- 0.005 ! need improvement Flux: V=5.99 +/- 0.02 B-V=0.57 +/- 0.02 Comments: Coordinates are from Hipparcos INCA Target_Number: 4 Target_Name: HD142373 Alternate_Names: GSC3057-02021, CHI-HER Description: STAR,F3-F9 Position: RA = 15H 52M 40.53S +/- 0.01S, DEC = 42D 27' 5.6" +/- 0.1", Equinox: J2000 RV_or_Z: V=-55 RA_PM: 0.0396 Dec_PM: 0.628 Epoch: 2000.000 Annual_Parallax: 0.056 +/- 0.005 Flux: V=4.62 +/- 0.02 B-V=0.56 +/- 0.02 Comments: Coordinates are from Hipparcos INCA Target_Number: 5 Target_Name: HD143761 Alternate_Names: GSC2576-02228, RHO-CRB Description: STAR,G V-IV Position: RA = 16H 01M 2.57S +/- 0.01S, DEC = 33D 18' 12.5" +/- 0.1", Equinox: J2000 RV_or_Z: V=18 RA_PM: -0.0159 Dec_PM: -0.768 Epoch: 2000.000 Annual_Parallax: 0.095 +/- 0.006 Flux: V=5.41 +/- 0.02 B-V=0.60 +/- 0.02 Comments: Coordinates are from Hipparcos INCA ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits ! Section 6 Visit_Number: 01 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: Exposure_Number: 10 ! Section 6.5 Target_Name: HD3651 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N2 Wavelength: Optional_Parameters: BRIGHT=RETURN, SEARCH-SIZE=3 Number_of_Iterations: 1 Time_Per_Exposure: 1.8S Special_Requirements: ONBOARD ACQ FOR 20 ! S 7.2 Comments: PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED (FOR COORDINATED OBSERVATIONS) IN ACQ EXPECT ABOUT 62000 CTS/S, HENCE STEP-TIME 0.2 SEC Exposure_Number: 15 ! Section 6.5 Target_Name: HD3651 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G270M Wavelength: 2800 Optional_Parameters: COMB=FOUR, STEP-PATT=DEF, DOPPLER=DEF, FP-SPLIT=STD Number_of_Iterations: 2 Time_Per_Exposure: 761.6S Special_Requirements: Comments: Line added to use up side 2 orbit Exposure_Number: 20 ! Section 6.5 Target_Name: HD3651 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1433.0 Optional_Parameters: COMB=FOUR, STEP-PATT=DEF, DOPPLER=DEF ! FP-SPLIT=STD Number_of_Iterations: 7 Time_Per_Exposure: 353.6S Special_Requirements: Comments: Visit_Number: 02 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: Exposure_Number: 10 ! Section 6.5 Target_Name: HD9562 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N1 Wavelength: Optional_Parameters: BRIGHT=RETURN, SEARCH-SIZE=3 Number_of_Iterations: 1 Time_Per_Exposure: 45S Special_Requirements: ONBOARD ACQ FOR 20 ! S 7.2 Comments: PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED (FOR COORDINATED OBSERVATIONS) IN ACQ EXPECT ABOUT 25 CTS/S, HENCE STEP-TIME 5 SEC Exposure_Number: 20 ! Section 6.5 Target_Name: HD9562 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1433.0 Optional_Parameters: COMB=FOUR, STEP-PATT=DEF, DOPPLER=DEF ! FP-SPLIT=STD Number_of_Iterations: 6 Time_Per_Exposure: 625.6S Special_Requirements: Comments: Visit_Number: 03 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: Exposure_Number: 10 ! Section 6.5 Target_Name: HD29645 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N1 Wavelength: Optional_Parameters: BRIGHT=RETURN, SEARCH-SIZE=3 Number_of_Iterations: 1 Time_Per_Exposure: 36S Special_Requirements: ONBOARD ACQ FOR 20 ! S 7.2 Comments: PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED (FOR COORDINATED OBSERVATIONS) IN ACQ EXPECT ABOUT 40 CTS/S, HENCE STEP-TIME 4 SEC Exposure_Number: 20 ! Section 6.5 Target_Name: HD29645 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1433.0 Optional_Parameters: COMB=FOUR, STEP-PATT=DEF, DOPPLER=DEF ! FP-SPLIT=STD Number_of_Iterations: 7 Time_Per_Exposure: 571.2S Special_Requirements: Comments: Visit_Number: 04 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: Exposure_Number: 10 ! Section 6.5 Target_Name: HD142373 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N1 Wavelength: Optional_Parameters: BRIGHT=RETURN, SEARCH-SIZE=3 Number_of_Iterations: 1 Time_Per_Exposure: 7.2S Special_Requirements: ONBOARD ACQ FOR 20 ! S 7.2 Comments: PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED (FOR COORDINATED OBSERVATIONS) IN ACQ EXPECT ABOUT 170 CTS/S, HENCE STEP-TIME 0.8 SEC Exposure_Number: 20 ! Section 6.5 Target_Name: HD142373 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1433.0 Optional_Parameters: COMB=FOUR, STEP-PATT=DEF, DOPPLER=DEF ! FP-SPLIT=STD Number_of_Iterations: 7 Time_Per_Exposure: 217.8S Special_Requirements: Comments: Visit_Number: 05 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: Exposure_Number: 10 ! Section 6.5 Target_Name: HD143761 Config: HRS Opmode: ACQ Aperture: 2.0 Sp_Element: MIRROR-N1 Wavelength: Optional_Parameters: BRIGHT=RETURN, SEARCH-SIZE=3 Number_of_Iterations: 1 Time_Per_Exposure: 18S Special_Requirements: ONBOARD ACQ FOR 20 ! S 7.2 Comments: PLEASE NOTIFY P.I. WHEN DATES ARE SCHEDULED OR CHANGED (FOR COORDINATED OBSERVATIONS) IN ACQ EXPECT ABOUT 70 CTS/S, HENCE STEP-TIME 2 SEC Exposure_Number: 20 ! Section 6.5 Target_Name: HD143761 Config: HRS Opmode: ACCUM Aperture: 2.0 Sp_Element: G140L Wavelength: 1433.0 Optional_Parameters: COMB=FOUR, STEP-PATT=DEF, DOPPLER=DEF ! FP-SPLIT=STD Number_of_Iterations: 5 Time_Per_Exposure: 272S Special_Requirements: Comments: Data_Distribution ! Defaults indicated; change if desired Medium: 8MM ! 8MM or 6250BPI or 1600BPI Blocking_Factor: 10 ! 10 or 1 ! Only astronomers with very old 9- ! track tape drives should consider ! a blocking factor of 1 Ship_To: PI_Address ! STSCI or PI_Address or ! PI Address from Phase I is: ! ! 60 Garden St. MS 58 Cambridge ! , MA 02138 ! ! Ship_Via: UPS ! UPS (2-day) or OVERNIGHT ! Overnight shipping done at PI expense Recipient_Email: ! Needed if Ship_To: is not PI_Address ! ! Let us know what you think of this template and software! ! Please send a list of your likes and dislikes to your Program Coordinator