A Curious History of Sunspot Penumbrae

TL;DR

This study analyzes historical sunspot data revealing how the penumbra-to-umbra area ratio varies with sunspot size and over time, providing insights into solar activity and sunspot structure.

Contribution

It presents a detailed historical analysis of sunspot penumbral ratios, highlighting systematic variations in small sunspots over nearly a century and their potential implications.

Findings

Penumbral to umbral area ratio increases with sunspot size.

Small sunspots show significant ratio fluctuations over time.

No abrupt changes linked to observational or personnel shifts.

Abstract

Daily records of sunspot group areas compiled by the Royal Observatory, Greenwich, from May of 1874 through 1976 indicate a curious history for the penumbral areas of the smaller sunspot groups. On average, the ratio of penumbral area to umbral area in a sunspot group increases from 5 to 6 as the total sunspot group area increases from 100 to 2000 microHem (a microHem is a millionth the area of a solar hemisphere). This relationship does not vary substantially with sunspot group latitude or with the phase of the sunspot cycle. However, for the sunspot groups with total areas <100 microHem, this ratio changes dramatically and systematically through this historical record. The ratio for these smallest sunspots is near 5.5 from 1874 to 1900. After a rapid rise to more than 7 in 1905 it drops smoothly to less than 3 by 1930 and then rises smoothly back to more than 7 in 1961. It then returns to near 5.5 from 1965 to 1976. The smooth variation from 1905 to 1961 shows no indication of any step-like changes that might be attributed to changes in equipment or personnel. The overall level of solar activity was increasing monotonically during this time period when the penumbra-to-umbra area ratio dropped to less than half its peak value and then returned. If this history can be confirmed by other observations (e.g., Mt. Wilson or Kodaikanal) it may impact our understanding of penumbra formation, our dynamo models, and our estimates of historical changes in the solar irradiance.