XRT: HOP 2 programs at East Limb
2007-09-27T00:11:24 to 2007-09-27T06:09:54
Science Goal: Polar Region Observation Campaign, Hinode/Canary Islands Campaign
Program: East_limb_C-poly_with_Gband
Target: QR
xcen=0 ycen=0
Instrument: XRT
HOP/JOP: 0
Description:
Daily Note: none
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 ??inner Hinode
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. ??Motivation: ?ENorth and south limb HINODE/SP data have shown a conspicuous presence of small magnetic fields structures that has not been detected up to now.?EThere is a strong interest in determining the magnetic structure and origin of these magnetic features, besides their relationship among the four cardinal points. ?EDisk center SP data have also shown a opulence of small scale flux tube concentrations with may be connected to north and south poles magnetic activity.Daily Note: none
Request to XRT HOP Number 0014: Quiet Sun magnetic fields: high cadence observation covering SOT FOV, with low temperature sensitive filters Active region magnetism: high cadence observation covering the active region
Other Instruments: VTT TIP: Stokes profiles in FeI 1.56 micron and MnI 1.52 micron TESOS+VIP: 2D Spectropolarimetry in Fe I 630nm THEMIS Fe I 630nm and Ca II IR triplet lines DOT: filtergrams in H alpha, CaII H, and G-band SST: magnetogram and G-band filtergram
Scientific Objectives: We are planning to carry out two kinds of study in this unique opportunity: characterization of quiet Sun magnetic fields including their evolution, and the study of moving magnetic features and flux cancellation events in sunspots. The two problems will be investigated using coordinated observations of Hinode and four solar telescopes in Canary Islands. SOT onboard Hinode and solar telescopes in Canary Islands (SST, VTT, THEMIS, and DOT) will allow us to perform perform high precision spectro-polarimetric measurements in different spectral ranges (in the photosphere and the chromosphere), and imaging observations at the highest spatial resolution possible. All layers of the solar atmosphere will be covered from the photosphere to the corona, by means of XRT and EIS onboard Hinode.Daily Note: none
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 ??inner Hinode
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. ??Motivation: ?ENorth and south limb HINODE/SP data have shown a conspicuous presence of small magnetic fields structures that has not been detected up to now.?EThere is a strong interest in determining the magnetic structure and origin of these magnetic features, besides their relationship among the four cardinal points. ?EDisk center SP data have also shown a opulence of small scale flux tube concentrations with may be connected to north and south poles magnetic activity.Daily Note: none
Request to XRT HOP Number 0014: Quiet Sun magnetic fields: high cadence observation covering SOT FOV, with low temperature sensitive filters Active region magnetism: high cadence observation covering the active region
Other Instruments: VTT TIP: Stokes profiles in FeI 1.56 micron and MnI 1.52 micron TESOS+VIP: 2D Spectropolarimetry in Fe I 630nm THEMIS Fe I 630nm and Ca II IR triplet lines DOT: filtergrams in H alpha, CaII H, and G-band SST: magnetogram and G-band filtergram
Scientific Objectives: We are planning to carry out two kinds of study in this unique opportunity: characterization of quiet Sun magnetic fields including their evolution, and the study of moving magnetic features and flux cancellation events in sunspots. The two problems will be investigated using coordinated observations of Hinode and four solar telescopes in Canary Islands. SOT onboard Hinode and solar telescopes in Canary Islands (SST, VTT, THEMIS, and DOT) will allow us to perform perform high precision spectro-polarimetric measurements in different spectral ranges (in the photosphere and the chromosphere), and imaging observations at the highest spatial resolution possible. All layers of the solar atmosphere will be covered from the photosphere to the corona, by means of XRT and EIS onboard Hinode.Daily Note: none
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 ??inner Hinode
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. ??Motivation: ?ENorth and south limb HINODE/SP data have shown a conspicuous presence of small magnetic fields structures that has not been detected up to now.?EThere is a strong interest in determining the magnetic structure and origin of these magnetic features, besides their relationship among the four cardinal points. ?EDisk center SP data have also shown a opulence of small scale flux tube concentrations with may be connected to north and south poles magnetic activity.Daily Note: none
Request to XRT HOP Number 0014: Quiet Sun magnetic fields: high cadence observation covering SOT FOV, with low temperature sensitive filters Active region magnetism: high cadence observation covering the active region
Other Instruments: VTT TIP: Stokes profiles in FeI 1.56 micron and MnI 1.52 micron TESOS+VIP: 2D Spectropolarimetry in Fe I 630nm THEMIS Fe I 630nm and Ca II IR triplet lines DOT: filtergrams in H alpha, CaII H, and G-band SST: magnetogram and G-band filtergram
Scientific Objectives: We are planning to carry out two kinds of study in this unique opportunity: characterization of quiet Sun magnetic fields including their evolution, and the study of moving magnetic features and flux cancellation events in sunspots. The two problems will be investigated using coordinated observations of Hinode and four solar telescopes in Canary Islands. SOT onboard Hinode and solar telescopes in Canary Islands (SST, VTT, THEMIS, and DOT) will allow us to perform perform high precision spectro-polarimetric measurements in different spectral ranges (in the photosphere and the chromosphere), and imaging observations at the highest spatial resolution possible. All layers of the solar atmosphere will be covered from the photosphere to the corona, by means of XRT and EIS onboard Hinode.Daily Note: none
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 ??inner Hinode
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. ??Motivation: ?ENorth and south limb HINODE/SP data have shown a conspicuous presence of small magnetic fields structures that has not been detected up to now.?EThere is a strong interest in determining the magnetic structure and origin of these magnetic features, besides their relationship among the four cardinal points. ?EDisk center SP data have also shown a opulence of small scale flux tube concentrations with may be connected to north and south poles magnetic activity.Daily Note: none
Request to XRT HOP Number 0014: Quiet Sun magnetic fields: high cadence observation covering SOT FOV, with low temperature sensitive filters Active region magnetism: high cadence observation covering the active region
Other Instruments: VTT TIP: Stokes profiles in FeI 1.56 micron and MnI 1.52 micron TESOS+VIP: 2D Spectropolarimetry in Fe I 630nm THEMIS Fe I 630nm and Ca II IR triplet lines DOT: filtergrams in H alpha, CaII H, and G-band SST: magnetogram and G-band filtergram
Scientific Objectives: We are planning to carry out two kinds of study in this unique opportunity: characterization of quiet Sun magnetic fields including their evolution, and the study of moving magnetic features and flux cancellation events in sunspots. The two problems will be investigated using coordinated observations of Hinode and four solar telescopes in Canary Islands. SOT onboard Hinode and solar telescopes in Canary Islands (SST, VTT, THEMIS, and DOT) will allow us to perform perform high precision spectro-polarimetric measurements in different spectral ranges (in the photosphere and the chromosphere), and imaging observations at the highest spatial resolution possible. All layers of the solar atmosphere will be covered from the photosphere to the corona, by means of XRT and EIS onboard Hinode.Daily Note: none
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 ??inner Hinode
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. ??Motivation: ?ENorth and south limb HINODE/SP data have shown a conspicuous presence of small magnetic fields structures that has not been detected up to now.?EThere is a strong interest in determining the magnetic structure and origin of these magnetic features, besides their relationship among the four cardinal points. ?EDisk center SP data have also shown a opulence of small scale flux tube concentrations with may be connected to north and south poles magnetic activity.Daily Note: none
Request to XRT HOP Number 0014: Quiet Sun magnetic fields: high cadence observation covering SOT FOV, with low temperature sensitive filters Active region magnetism: high cadence observation covering the active region
Other Instruments: VTT TIP: Stokes profiles in FeI 1.56 micron and MnI 1.52 micron TESOS+VIP: 2D Spectropolarimetry in Fe I 630nm THEMIS Fe I 630nm and Ca II IR triplet lines DOT: filtergrams in H alpha, CaII H, and G-band SST: magnetogram and G-band filtergram
Scientific Objectives: We are planning to carry out two kinds of study in this unique opportunity: characterization of quiet Sun magnetic fields including their evolution, and the study of moving magnetic features and flux cancellation events in sunspots. The two problems will be investigated using coordinated observations of Hinode and four solar telescopes in Canary Islands. SOT onboard Hinode and solar telescopes in Canary Islands (SST, VTT, THEMIS, and DOT) will allow us to perform perform high precision spectro-polarimetric measurements in different spectral ranges (in the photosphere and the chromosphere), and imaging observations at the highest spatial resolution possible. All layers of the solar atmosphere will be covered from the photosphere to the corona, by means of XRT and EIS onboard Hinode.
