2007-05-16T20:42:46.000Z http://sot.lmsal.com Mr. Sam Freeland Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) http://www.lmsal.com Lockheed Martin Advanced Tech Center, 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA 94304 null null Hinode XRT Hara Sterling, A. Ishibashi, B 0 Active region tracking across disk AR AR, SS 10955 2 598.252 -105.23 2113.54 2113.54 2007-05-14T06:24:04.000Z 2007-05-14T18:05:38.000Z 598.252 -105.23 CDS/UVCS + Ulysses Campaign AR_on_disk_11 Tim File-OBS_DEC: AR - Microflares and Topology - Ti/Poly, Thick-Al, Thick-Be pairs, G-band - contexts + 512 - high cadence; Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun).Daily Note: XRT: STEREO campaign; SOHO/UCVS-Ulysses campaign, and will do 12-filter scan during EIS cal. EIS: Calibration run over weekend. EIS: 1) UVCS-Ulysses campaign: Abundances as function of height in AR. EIS is requested to observe AR at the limb for a min of 4 hr 15 min per day on five days spanning west limb passage [7th May to disappearance of AR] 2) STEREO campaign. EIS will raster the slit across the active region on the disc and at the limb. (STEREO/SECCHI will complement with 75-second cadence 171 filtergrams, with other three wavelengths at 5-minute cadence.) [4th to 8th May] 3) Coronal dimming study. EIS will run coronal_wave_study to look for evidence of dimming following large events if activity looks likely. [As long as AR is visible] 4) After disappearance of the AR, EIS would like quiet Sun pointing near limb for: a) line broadening and diagnostics above limb b) STEREO campaign 304 high-cadence co-observations of spicules c) UVCS campaign If co-alignment program (2hr for N-limb, 2hr for E-limb) was not included in the May 5-7 weekend plan, please run this program soon after disappearance of the AR. andnbsp;This run will be important for calibrating absolute heliocentric coordinate for quiet sun. Also, this program may run once every a few days, depending on the satellite temperatures and science programs.; Request to XRT HOP Number 0007: ; Other Instruments: SoHO/CDS, UVCS; SoHO keyhole starts 17-May (26m dish) and 21-May (34m dish) STEREO/SECCHI Ulysses will be ending the quadrature with SOHO. Ulysses will be at a latitude of 55 deg (south-west), in the plane of the sky. Hence any active region say between 45 and 65 degree south that might be near the limb would contribute to the solar wind measured in-situ by Ulysses. Scintillation measurement (G. Poletto); Scientific Objectives: The main aim is to measure chemical abundances in active regions as a function of height for 1.0 andlt; R(Sun) andlt; 1.6 using SOHO/CDS, Hinode/EIS, SOHO/UVCS, and to link them with in-situ measurements by Ulysses. A secondary aim is to measure electron temperatures, densities, and ionization state of the plasma as function of height from 1.0 to 1.6 solar radii using SOHO/CDS and Hinode/EIS. There have been no previous spectroscopic observations in the range 1.2 and;#8211; 1.6 R(Sun). ivo://sot.lmsal.com/VOEvent#2007-05-14T06:21:54Z