XRT: AR Evolution No darks 768x512
2007-01-14T10:11:30 to 2007-01-14T15:50:30
Science Goal: Polar Region Observation Campaign
Program: AR_Evolution_765x512_ROI_North_Pole_3
Target: AR
xcen=74 ycen=-978
Instrument: XRT
HOP/JOP: 0
Description:
Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Weekly Meeting Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Weekly Meeting Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Weekly Meeting Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Weekly Meeting Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Weekly Meeting Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Weekly Meeting Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Weekly Meeting Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Weekly Meeting Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Weekly Meeting Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.Daily Note: Joint XRT, EIS, SOT, SOHO polar observations are requested, beginning on Tuesday, 2007/01/09. andnbsp
XRT proposes polar observations for six hours each day of the week, between usual synoptics at 16:00UT and 22:00UT. andnbsp
XRT requests a data rate of 22.5%. Data Rate: SOT 62.5%, XRT 22.5%, EIS 15% Continue to track the active region, except above synoptic and polar observation time.
Request to XRT HOP Number 0002: High cadence observations in a single filter (Al-poly) with a 1024 x 384 field of view. 16.34 sec exposures have already been tested for this type observation. Also, context images with a field of view of 1024 x 960 (offset relative to the pointing position) are required to extend the field of view to 0.7 solar radii. This is the expected slit position of the UVCS instrument on SoHO.
Other Instruments: UVCS: spectral line intensities for doppler dimming and velocity measurements with a slit position orthogonal to solar north CDS: Observations with the 2"" slit using the line list in JOP 146. It would be useful to use the same
slit positions as EIS. TRACE: 1711 1024 x 1024, Q4 @ 30s cadence with 1600 or 1550 and
WL in context. LASCO: TBD
Scientific Objectives: Objective: To characterize the temperature, dynamics and statistical distribution of polar coronal jets recently observed by XRT. Scientific Justification: Recent observations of the north polar coronal hole have shown highly dynamic and frequent (numerous per hour) x-ray jets. This apparently originate from small ephemeral regions within and near the coronal hole boundary. These jets may be the final phase of reconnection
produced when a bi-pole emerges into a predominately open flux region. The previous observations of XRT, taken on 23 November 2006, capture some 44 of these events in a roughly 6 hour period. Estimates of the mass-loading into the IMF based upon a density assumption of 10^9 and volume put the mass flux at just under an order of magnitude of the fast solar wind. These two realizations, the so-called 'Shibata-type' reconnection events and the contribution of mass to the solar wind, are sufficient justification for this observation request.
Jibben, Patricia, R.
