This article is a commentary about the state of Integrated, Coordinated, Open, and Networked (ICON) principles (Goldman et al., 2021) in Space Physics and Aeronomy and a discussion on several scopes and limitations to implementing them. The commentary focuses on the basic introduction and brief literature survey (Section 1); possibilities of implementation of ICON in Space Physics and Aeronomy (Section 2) and limitations or challenges in this field with possible solutions using ICON principles (Section 3). The Space Physics and Aeronomy section of the American Geophysical Union (AGU) comprises the interactions between solar wind, Interplanetary Magnetic Field (IMF) and different planetary magnetospheres and ionospheres. The section also deals with solar physics, mechanisms behind existence of solar magnetic fields, and evaluations of high and low speed solar winds. This field is a collection of different interdisciplinary subtopics, making this an excellent example of integrated research. Similar and transparent methodologies are adopted to solve problems all over the world which shows a coordinated approach of research. Freely available data from different space agencies and universities are also great assets for this domain which supports open research. The scopes of possible networked research with mutual benefits are also highlighted. Examples of ICON-based international collaborations and support mechanisms towards young scientists are elaborated which are helpful to mitigate limitations in this domain.

The paper inspects the effects of a G2 class geomagnetic storm that occurred during 27 February- 1 March, 2014 on the equatorial ionization. This storm is observed following a Coronal Mass Ejection (CME) from a sunspot AR1967 on 26 February. An enhancement of solar wind speed is observed on 27 February, 2014 (483 km/sec). The maximum southward component of Interplanetary Magnetic Field (IMF) is observed around 21 UT of 27 February (12 nT). This interconnects with Earth’s magnetic field and develops the main phase of a geomagnetic storm on the same day. The storm continues through 28 February and quiet-time ionospheric condition is recovered on 1 March. The effects of the storm on equatorial ionization is observed at Brasilia (15.95°S, 47.88°W geographic; 9.40°N, 21.13°E geomagnetic), Addis Ababa (9.04°N, 38.77°E geographic; 0.18°N, 110.47°E geomagnetic) and Colombo (6.89°N, 79.87°E geographic; 1.57°S, 151.57°E geomagnetic). An enhancement of TEC is observed during main phase of the geomagnetic storm at these stations. Increment in diurnal peak is observed on 28 February (14 TECU at 10 UT at Addis Ababa) while a decrement of diurnal peak TEC is observed during the recovery phase of the storm (15 TECU at 10 UT at Addis Ababa). Post-sunset ionospheric scintillation is inhibited at Brasilia on 28 February.