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HINODE Operation Plan (HOP)

accepted on

14-jan-2021


 HOP No.

 HOP title

HOP 0412

Synoptic SOT Latitudinal Scans (updated version of HOP79)

plan term

2021/02/18-2021/02/18
2021/03/18-2021/03/18
2021/04/15-2021/04/15
2021/05/20-2021/05/20
2021/06/17-2021/06/17
2021/07/16-2021/07/16
2021/08/12-2021/08/12
2021/09/29-2021/09/29
2021/10/28-2021/10/28
2021/11/18-2021/11/18
2021/12/16-2021/12/16
2022/03/24-2022/03/24
2022/04/14-2022/04/14
2022/05/19-2022/05/19
2022/06/09-2022/06/09
2022/07/21-2022/07/21
2022/08/17-2022/08/17
2022/09/22-2022/09/22
2022/10/20-2022/10/20
2022/11/17-2022/11/17
2022/12/28-2022/12/28
2023/01/12-2023/01/12
2023/02/16-2023/02/16
2023/03/24-2023/03/24
2023/04/21-2023/04/21
2023/05/18-2023/05/18
2023/06/22-2023/06/22
2023/07/20-2023/07/20
2023/08/17-2023/08/17
2023/09/21-2023/09/21
2023/10/19-2023/10/19
2023/11/03-2023/11/03
2023/11/16-2023/11/16
2023/12/14-2023/12/14
2024/01/11-2024/01/11
2024/02/15-2024/02/15
2024/03/14-2024/03/14
2024/04/18-2024/04/18
2024/05/16-2024/05/16
2024/06/20-2024/06/20
2024/07/18-2024/07/18
2024/08/15-2024/08/15

@ @

proposer

 name : Egeland, Centeno @  e-mail : egeland[at]ucar.edu, rce[at]ucar.edu

contact person in HINODE team

 name : DeRosa, Shine
@  e-mail : derosa[at]lmsal.com, shine[at]lmsal.com

 abstract of observational proposal
Main Objective: To study how small-scale magnetic flux and solar irradiance varies over the sunspot cycle

Scientific Justification: The total solar irradiance varies by about 0.1% over the course of the solar cycle, primarily due to the influence of magnetic structures such as sunspots and faculae on the photospheric spectral irradiance. Short-term irradiance variation (on the scale of days-to-months) is well understood to be due to the balance of sunspots and facular areas as they cross the disk. However on the decadal scale of the solar cycle, questions remain as to why the irradiance variation can lead and/or lag the active region count over the course of the cycle. Explanations ranging from changes inthe solar diameter in response to magnetic flux storage in the convection zone to changes in the surface area of the photosphere due to F-mode modulation have been put forward.

We propose to observe a north-to-south latitudinal strip with SOT-SP on a regular basis to better understand the variation of irradiance with rising flux levels in the photosphere. These observations have the potential to reveal new and important aspects of the relation between solar irradiance and magnetic flux emergence over the solar cycle when compared with TSI measurement satellites such as TSIS-1 and TSIS-2.

In addition, work by Shiozu and Tsuneta has shown that HOP 79 N-S scan scan data can be used to infer the latitudinal temperature variation between the equator and the poles thus offering constraints on "thermal wind" theories of convection zone rotational profiles. Lites, Centeno, and McIntosh 2014 analyzed the north-to-south latitudinal strip with SOT/SP (HOP79) for the period Nov 2008 to May 2013, the rising phase of Cycle 24. They found that the smallest scale flux did not appear to vary along with the large-scale flux of the cycle, while a polarity transition at the polar region was observed. Further synoptic observations can be used to compare changes in small-scale flux along the meridian for a second solar minimum period, as well as for Cycle 25 which could potentially be stronger than Cycle 24.

 request to SOT

 request to XRT

 request to EIS

 other participating instruments

 remarks
Dates: once per month, as HOP79

Time window: once per month, as HOP79

Target(s) of interest: central meridian

IRIS requests
None

Additional instrument coordination
None

Previous HOPs
HOP79

Additional remarks
This HOP is done regardless of solar activity - it is *not* a quiet Sun HOP and it is acceptable to include active regions in the view fields.

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