2007-09-02T23:36:41.000Z 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 KANO, Ryohei ISHIBASHI, Kazunori 0 16 739.13 -148.753 528.415 528.415 2007-08-31T00:54:29.000Z 2007-08-31T15:37:12.000Z 739.13 -148.753 Polar Region Observation Campaign, Determination of the properties of families of solar granules and formation of the photospheric network, Active Region and; Network Wave Propagation: Active Region Movie STOP_START_Observation Tim File-OBS_DEC: CCD Monitor During Bakeout - G-Band and X-ray + 4 strips Al/mesh; 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 0021: We are also interested, if the Hinode rate allows it, to get observations with EIS and XRT every 10 or 20 minutes of the same field of view. This will help to follow the hot corona (Al_Poly Filter) with XRT, during the formation of the photospheric network in the quiet Sun.; Other Instruments: Pic du Midi CALAS; Scientific Objectives: The main goal of our proposal is to study the families of granules and the photospheric network formation by these families during a long time sequence 24 to 48 hours if possible. We also plan to observe at the same time (3 to 6 hours) from Pic du Midi over a large field of view (10?fx10?f) in ;the G-band with our 4kx4k CMOS camera CALAS (http://ljr.bagn.obs-mip.fr/calas/index.html). The observed families will be compared with the families generated by our new simulation code of the solar granulation developed in our team. We plan also to improve a posteriori ground observation over a large field of view by using simultaneous G-band SOT observations free from atmospheric seeing. Daily Note: none; Request to XRT HOP Number 0034: XRT observations are requested to provide 'Dynamics' observations. High cadence 512x512, no binning, observations are requested in the Ti_poly filter with 20s exposure and ~30s cadence, or alternatively 368x368 images if required to obtain high cadence.; Other Instruments: SST TRACE; Scientific Objectives: Intensity and velocity oscillations have been observed in the chromosphere above sunspots for over thirty years (Beckers and; Tallant 1969; Beckers and; Schultz 1972; Gurman et al. 1982; Lites et al. 1982). These oscillations have since been observed in the transition region, using space-based instruments observing in the extreme ultra-violet (EUV) (see, Fludra 2001; O'Shea et al. 2002; Rendtel et al. 2003; Brynildsen et al. 2004, and references within). Additionally, space-based EUV bandpass imagers have observed periodic intensity propagations along diffuse, fan-like, coronal loop structures (Berghmans and; Clette 99; Nightingale et al 1999, De Moortel 2002a). De Moortel (2002b) observe a relationship between 3-minute propagations found within sunspot coronal loops, and 5-minute propagations found within plage coronal loops. In Marsh et al.(2003) we present an observation of a 5-minute propagating wave within a plage coronal loop; the intensity oscillation of the wave was also observed simultaneously at transition region temperatures, suggesting wave propagation through the transition region into the corona along the active region loops. Depontieu et al. (2005) also discuss the possibility of channeling the 5-min photospheric oscillations into the corona along the magnetic field. The bright solar network, defined by the boundaries of supergranular flows, is dominated by magnetohydrodynamic (MHD) processes and contains oscillations with periods above of the acoustic cut-off (Goodman 2000). Regions of enhanced emission have the strongest magnetic fields and constitute the most intense radiative losses. The microstructure of these fields and their interactions with the convection zone supply energy to the overlying layers. The granular buffeting of flux tubes in the photosphere can create transverse waves which may mode couple to longitudinal waves and can be observed through variations in the plasma emission and radial velocity. In Marsh and; Walsh (2006) we present new, spatially resolved, monochromatic imaging data of a sunspot region at transition region temperatures, combined with simultaneous bandpass imaging of the emerging coronal loops. The 3-minute umbral oscillations are observed in the transition region, and are then observed to propagate along the sunspot coronal loop system. These propagating waves are interpreted as the transmission of global p-modes that undergo absorption, slow mode conversion, and are wave-guided into the corona by the strong magnetic field. A complete, simultaneous, view of the atmosphere from the photosphere, chromosphere, transition region and corona is required.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 0021: We are also interested, if the Hinode rate allows it, to get observations with EIS and XRT every 10 or 20 minutes of the same field of view. This will help to follow the hot corona (Al_Poly Filter) with XRT, during the formation of the photospheric network in the quiet Sun.; Other Instruments: Pic du Midi CALAS; Scientific Objectives: The main goal of our proposal is to study the families of granules and the photospheric network formation by these families during a long time sequence 24 to 48 hours if possible. We also plan to observe at the same time (3 to 6 hours) from Pic du Midi over a large field of view (10?fx10?f) in ;the G-band with our 4kx4k CMOS camera CALAS (http://ljr.bagn.obs-mip.fr/calas/index.html). The observed families will be compared with the families generated by our new simulation code of the solar granulation developed in our team. We plan also to improve a posteriori ground observation over a large field of view by using simultaneous G-band SOT observations free from atmospheric seeing. Daily Note: none; Request to XRT HOP Number 0034: XRT observations are requested to provide 'Dynamics' observations. High cadence 512x512, no binning, observations are requested in the Ti_poly filter with 20s exposure and ~30s cadence, or alternatively 368x368 images if required to obtain high cadence.; Other Instruments: SST TRACE; Scientific Objectives: Intensity and velocity oscillations have been observed in the chromosphere above sunspots for over thirty years (Beckers and; Tallant 1969; Beckers and; Schultz 1972; Gurman et al. 1982; Lites et al. 1982). These oscillations have since been observed in the transition region, using space-based instruments observing in the extreme ultra-violet (EUV) (see, Fludra 2001; O'Shea et al. 2002; Rendtel et al. 2003; Brynildsen et al. 2004, and references within). Additionally, space-based EUV bandpass imagers have observed periodic intensity propagations along diffuse, fan-like, coronal loop structures (Berghmans and; Clette 99; Nightingale et al 1999, De Moortel 2002a). De Moortel (2002b) observe a relationship between 3-minute propagations found within sunspot coronal loops, and 5-minute propagations found within plage coronal loops. In Marsh et al.(2003) we present an observation of a 5-minute propagating wave within a plage coronal loop; the intensity oscillation of the wave was also observed simultaneously at transition region temperatures, suggesting wave propagation through the transition region into the corona along the active region loops. Depontieu et al. (2005) also discuss the possibility of channeling the 5-min photospheric oscillations into the corona along the magnetic field. The bright solar network, defined by the boundaries of supergranular flows, is dominated by magnetohydrodynamic (MHD) processes and contains oscillations with periods above of the acoustic cut-off (Goodman 2000). Regions of enhanced emission have the strongest magnetic fields and constitute the most intense radiative losses. The microstructure of these fields and their interactions with the convection zone supply energy to the overlying layers. The granular buffeting of flux tubes in the photosphere can create transverse waves which may mode couple to longitudinal waves and can be observed through variations in the plasma emission and radial velocity. In Marsh and; Walsh (2006) we present new, spatially resolved, monochromatic imaging data of a sunspot region at transition region temperatures, combined with simultaneous bandpass imaging of the emerging coronal loops. The 3-minute umbral oscillations are observed in the transition region, and are then observed to propagate along the sunspot coronal loop system. These propagating waves are interpreted as the transmission of global p-modes that undergo absorption, slow mode conversion, and are wave-guided into the corona by the strong magnetic field. A complete, simultaneous, view of the atmosphere from the photosphere, chromosphere, transition region and corona is required.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 0021: We are also interested, if the Hinode rate allows it, to get observations with EIS and XRT every 10 or 20 minutes of the same field of view. This will help to follow the hot corona (Al_Poly Filter) with XRT, during the formation of the photospheric network in the quiet Sun.; Other Instruments: Pic du Midi CALAS; Scientific Objectives: The main goal of our proposal is to study the families of granules and the photospheric network formation by these families during a long time sequence 24 to 48 hours if possible. We also plan to observe at the same time (3 to 6 hours) from Pic du Midi over a large field of view (10?fx10?f) in ;the G-band with our 4kx4k CMOS camera CALAS (http://ljr.bagn.obs-mip.fr/calas/index.html). The observed families will be compared with the families generated by our new simulation code of the solar granulation developed in our team. We plan also to improve a posteriori ground observation over a large field of view by using simultaneous G-band SOT observations free from atmospheric seeing. Daily Note: none; Request to XRT HOP Number 0034: XRT observations are requested to provide 'Dynamics' observations. High cadence 512x512, no binning, observations are requested in the Ti_poly filter with 20s exposure and ~30s cadence, or alternatively 368x368 images if required to obtain high cadence.; Other Instruments: SST TRACE; Scientific Objectives: Intensity and velocity oscillations have been observed in the chromosphere above sunspots for over thirty years (Beckers and; Tallant 1969; Beckers and; Schultz 1972; Gurman et al. 1982; Lites et al. 1982). These oscillations have since been observed in the transition region, using space-based instruments observing in the extreme ultra-violet (EUV) (see, Fludra 2001; O'Shea et al. 2002; Rendtel et al. 2003; Brynildsen et al. 2004, and references within). Additionally, space-based EUV bandpass imagers have observed periodic intensity propagations along diffuse, fan-like, coronal loop structures (Berghmans and; Clette 99; Nightingale et al 1999, De Moortel 2002a). De Moortel (2002b) observe a relationship between 3-minute propagations found within sunspot coronal loops, and 5-minute propagations found within plage coronal loops. In Marsh et al.(2003) we present an observation of a 5-minute propagating wave within a plage coronal loop; the intensity oscillation of the wave was also observed simultaneously at transition region temperatures, suggesting wave propagation through the transition region into the corona along the active region loops. Depontieu et al. (2005) also discuss the possibility of channeling the 5-min photospheric oscillations into the corona along the magnetic field. The bright solar network, defined by the boundaries of supergranular flows, is dominated by magnetohydrodynamic (MHD) processes and contains oscillations with periods above of the acoustic cut-off (Goodman 2000). Regions of enhanced emission have the strongest magnetic fields and constitute the most intense radiative losses. The microstructure of these fields and their interactions with the convection zone supply energy to the overlying layers. The granular buffeting of flux tubes in the photosphere can create transverse waves which may mode couple to longitudinal waves and can be observed through variations in the plasma emission and radial velocity. In Marsh and; Walsh (2006) we present new, spatially resolved, monochromatic imaging data of a sunspot region at transition region temperatures, combined with simultaneous bandpass imaging of the emerging coronal loops. The 3-minute umbral oscillations are observed in the transition region, and are then observed to propagate along the sunspot coronal loop system. These propagating waves are interpreted as the transmission of global p-modes that undergo absorption, slow mode conversion, and are wave-guided into the corona by the strong magnetic field. A complete, simultaneous, view of the atmosphere from the photosphere, chromosphere, transition region and corona is required.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 0021: We are also interested, if the Hinode rate allows it, to get observations with EIS and XRT every 10 or 20 minutes of the same field of view. This will help to follow the hot corona (Al_Poly Filter) with XRT, during the formation of the photospheric network in the quiet Sun.; Other Instruments: Pic du Midi CALAS; Scientific Objectives: The main goal of our proposal is to study the families of granules and the photospheric network formation by these families during a long time sequence 24 to 48 hours if possible. We also plan to observe at the same time (3 to 6 hours) from Pic du Midi over a large field of view (10?fx10?f) in ;the G-band with our 4kx4k CMOS camera CALAS (http://ljr.bagn.obs-mip.fr/calas/index.html). The observed families will be compared with the families generated by our new simulation code of the solar granulation developed in our team. We plan also to improve a posteriori ground observation over a large field of view by using simultaneous G-band SOT observations free from atmospheric seeing. Daily Note: none; Request to XRT HOP Number 0034: XRT observations are requested to provide 'Dynamics' observations. High cadence 512x512, no binning, observations are requested in the Ti_poly filter with 20s exposure and ~30s cadence, or alternatively 368x368 images if required to obtain high cadence.; Other Instruments: SST TRACE; Scientific Objectives: Intensity and velocity oscillations have been observed in the chromosphere above sunspots for over thirty years (Beckers and; Tallant 1969; Beckers and; Schultz 1972; Gurman et al. 1982; Lites et al. 1982). These oscillations have since been observed in the transition region, using space-based instruments observing in the extreme ultra-violet (EUV) (see, Fludra 2001; O'Shea et al. 2002; Rendtel et al. 2003; Brynildsen et al. 2004, and references within). Additionally, space-based EUV bandpass imagers have observed periodic intensity propagations along diffuse, fan-like, coronal loop structures (Berghmans and; Clette 99; Nightingale et al 1999, De Moortel 2002a). De Moortel (2002b) observe a relationship between 3-minute propagations found within sunspot coronal loops, and 5-minute propagations found within plage coronal loops. In Marsh et al.(2003) we present an observation of a 5-minute propagating wave within a plage coronal loop; the intensity oscillation of the wave was also observed simultaneously at transition region temperatures, suggesting wave propagation through the transition region into the corona along the active region loops. Depontieu et al. (2005) also discuss the possibility of channeling the 5-min photospheric oscillations into the corona along the magnetic field. The bright solar network, defined by the boundaries of supergranular flows, is dominated by magnetohydrodynamic (MHD) processes and contains oscillations with periods above of the acoustic cut-off (Goodman 2000). Regions of enhanced emission have the strongest magnetic fields and constitute the most intense radiative losses. The microstructure of these fields and their interactions with the convection zone supply energy to the overlying layers. The granular buffeting of flux tubes in the photosphere can create transverse waves which may mode couple to longitudinal waves and can be observed through variations in the plasma emission and radial velocity. In Marsh and; Walsh (2006) we present new, spatially resolved, monochromatic imaging data of a sunspot region at transition region temperatures, combined with simultaneous bandpass imaging of the emerging coronal loops. The 3-minute umbral oscillations are observed in the transition region, and are then observed to propagate along the sunspot coronal loop system. These propagating waves are interpreted as the transmission of global p-modes that undergo absorption, slow mode conversion, and are wave-guided into the corona by the strong magnetic field. A complete, simultaneous, view of the atmosphere from the photosphere, chromosphere, transition region and corona is required.