Editing Sunspot (section)

==== Formation ====
Although the details of sunspot formation are still a matter of ongoing research, it is widely understood that they are the visible manifestations of [[magnetic flux tube]]s in the Sun's [[convective zone]] projecting through the photosphere within active regions.<ref name="solanki03">{{cite journal |last1=Solanki |first1=Sami K. |title=Sunspots: An overview |journal=Astronomy and Astrophysics Review |date=1 April 2003 |volume=11 |issue=2–3 |pages=153–286 |doi=10.1007/s00159-003-0018-4|bibcode=2003A&ARv..11..153S |s2cid=120721248 }}</ref> Their characteristic darkening occurs due to this strong magnetic field inhibiting [[convection]] in the photosphere. As a result, the energy flux from the Sun's interior decreases, and with it, surface temperature, causing the surface area through which the magnetic field passes to look dark against the bright background of [[Granule (solar physics)|photospheric granules]].

Sunspots initially appear in the photosphere as small darkened spots lacking a penumbra. These structures are known as solar pores.<ref>{{cite journal |last1=Sobotka |first1=Michal |last2=Vazquez |first2=Manuel |last3=Bonet |first3=Jose Antonio |last4=Hanslmeier |first4=Arnold |last5=Hirzberger |first5=Johann |title=Temporal Evolution of Fine Structures in and around Solar Pores |journal=The Astrophysical Journal |date=20 January 1999 |volume=511 |issue=1 |pages=436–450 |doi=10.1086/306671 |bibcode=1999ApJ...511..436S |s2cid=121691780 |url=https://iopscience.iop.org/0004-637X/511/1/436/pdf/0004-637X_511_1_436.pdf |access-date=5 January 2022}}</ref> Over time, these pores increase in size and move towards one another. When a pore gets large enough, typically around {{convert|3500|km|mi|sigfig=1|sp=us|abbr=on}} in diameter, a penumbra will begin to form.<ref name="solanki03" />