Alfvénic slow wind is a strange beast. First observed by Helios, it has only been confirmed within the last decade and has challenged our usual understanding and classification of solar wind streams. With a high absolute cross-helicity, indicating an imbalanced proportion of outward Alfvén waves, it resembles the coronal hole fast wind. It could thus find its origin in the core of very rapidly expanding small coronal holes that are known to give birth to slower and denser wind streams. Close to the Sun, Parker Solar Probe and Solar Orbiter have found many examples of such streams that seem less likely to survive up to 1 AU. In this work, we focus on a series of slow Alfvénic wind streams followed by a fast wind stream observed by Solar Orbiter between March and April 2022. We study the sources of the solar wind through PFSS extrapolations of the photospheric magnetic field observed from different sources, and with a full MHD model, driven by Alfvén wave turbulence. We compare the sources and expansion properties provided by the two models and find similar results, although the expansion given by the PFSS is generally overestimated. Then, we study the heating and acceleration profile in the MHD model. We compare the Alfvénic turbulence heating with expansion dependent heating function and show that atypical non-monotonic acceleration profile can be the source of slow alfvénic streams. Finally, we examine the quasi-sepatrix network and try to assess whether it can also be a source of slow Alfvénic streams during this interval.