@Article{Muñoz-JaramilloSLTPBDM:2015:DeItCo,
author = "Muñoz-Jaramillo, Andr{\'e}s and Senkpeil, Ryan R. and Longcope,
Dana W. and Tlatov, Andrey G. and Pevtsov, Alexei A. and
Balmaceda, Laura Antonia and DeLuca, Edward E. and Martens, Petrus
C. H.",
affiliation = "{Montana State University} and {Purdue University} and {Montana
State University} and {Kislovodsk Mountain Astronomical Station of
the Pulkovo Observatory} and {National Solar Observatory} and
{Instituto Nacional de Pesquisas Espaciais (INPE)} and
{Harvard-Smithsonian Center for Astrophysics} and {Georgia State
University}",
title = "The minimum of solar cycle 23: as deep as it could be?",
journal = "The Astrophysical Journal",
year = "2015",
volume = "804",
number = "68",
keywords = "Sun: activity – Sun: magnetic fields – Sun: photosphere –
sunspots.",
abstract = "In this work we introduce a new way of binning sunspot group data
with the purpose of better understanding the impact of the solar
cycle on sunspot properties and how this defined the
characteristics of the extended minimum of cycle 23. Our approach
assumes that the statistical properties of sunspots are completely
determined by the strength of the underlying large-scale field and
have no additional time dependencies. We use the amplitude of the
cycle at any given moment (something we refer to as activity
level) as a proxy for the strength of this deep-seated magnetic
field. We find that the sunspot size distribution is composed of
two populations: one population of groups and active regions and a
second population of pores and ephemeral regions. When fits are
performed at periods of different activity level, only the
statistical properties of the former population, the active
regions, are found to vary. Finally, we study the relative
contribution of each component (small-scale versus large-scale) to
solar magnetism. We find that when hemispheres are treated
separately, almost every one of the past 12 solar minima reaches a
point where the main contribution to magnetism comes from the
small-scale component. However, due to asymmetries in cycle phase,
this state is very rarely reached by both hemispheres at the same
time. From this we infer that even though each hemisphere did
reach the magnetic baseline, from a heliospheric point of view the
minimum of cycle 23 was not as deep as it could have been.",
doi = "10.1088/0004-637X/804/1/68",
url = "http://dx.doi.org/10.1088/0004-637X/804/1/68",
issn = "0004-637X",
language = "en",
urlaccessdate = "27 abr. 2024"
}