Interplanetary Tracking of the 23 March 2024 CME: Computer Tomographic Analyses of IPS, White‐Light, and Type II Radio Burst Observations

Abstract We analyze the propagation of a coronal mass ejection (CME) observed on 23 March 2024, at 01:25 UT by SOHO/LASCO using a multi‐instrument and multi‐method approach. The study combines Interplanetary Scintillation (IPS), type II radio bursts, white‐light, in‐situ observations, and 3D tomographic reconstruction of the inner heliospheric density. The associated shock was detected in the metric range by the CALLISTO Australia‐ASSA station and in the interplanetary medium by STEREO/SWAVES. IPS observations from LOw Frequency ARray (LOFAR) and Mexican Array Radio Telescope (MEXART) were used to estimate solar wind speeds, while spectral analysis of type II emissions provided the radial velocity of the coronal shock. Additionally, kilometric type II emissions were analyzed to track the CME‐driven shock through interplanetary space. The UCSD team produced 3D reconstructions of the heliospheric density distribution in conjunction with STEREO‐A observations. Our results indicate that STEREO‐A recorded an ejection size ∼0.51 AU, with a transit time of about 37 hr. The lack of CME detection by SOHO/CELIAS indicates non‐radial propagation, supported by 3D reconstruction. IPS observations showed enhanced solar wind speeds from radio sources northeast of the Sun‐Earth line, ranging from 600 to 1,000 km/s. Using the lower edge of the type II emission band offers a good estimate of the shock's arrival time, which can be refined with time‐distance data from SOHO/LASCO and Solar Orbiter (SolO). This combined approach gives a consistent description of CME evolution from the Sun to 1 AU.