The Sun has a 4.6 Gyr long history which was subject to numerous investigations. The “Sun in time” program (see e.g. Dorren & Guinan 1994; Güdel 2007) was founded to investigate the Sun’s history in great detail. The radiation environment was reconstructed from X-rays (e.g. Dorren et al. 1995; Güdel et al. 1997b; Telleschi et al. 2005; Guinan 2017), EUV (e.g. Güdel et al. 1997a; Tu et al. 2015), FUV (e.g. Guinan et al. 2003), UV (e.g. Dorren & Guinan 1994; Dalton et al. 2019), optical (e.g. Messina & Guinan 2002) to radio (e.g. Güdel et al. 1994; Villadsen et al. 2014; Fichtinger et al. 2017). The spectral energy distributions of the Sun in time has been inferred (Ribas et al. 2005; Claire et al. 2012) and also the solar wind in time has been investigated (Ó Fionnagáin & Vidotto 2018). Every study focusing on solar analogues of different age may be attributed to the idea of the “Sun in time” program. Transient activity phenomena like flares and CMEs of the young Sun can be characterized with a significant observational effort only as those are detectable via time series observations which require much observing time. Here, especially the CME environment of the young Sun remains still relatively unknown. However, flare frequency distributions, as well as flare power laws depending on the stars X-ray luminosity of young solar analogue stars and others have been presented by Audard et al. (2000). Based on these power laws Odert et al. (2017) have deduced relations to estimate stellar CME occurrence rates. Prior to Odert et al. (2017), Aarnio et al. (2012) established a methodology to relate solar flare/CME relations with stellar flaring relations to infer stellar CMEs and their parameters. Drake et al. (2013) applied a similar approach and identified the problem of the unknown stellar flare-CME association rate, as extrapolating to higher energies while using solar relations leads to unrealistic high energy requirements which have been not observed yet. Osten & Wolk (2015) assumed energy partition between bolometric flare radiation and kinetic energy of the associated CME. These authors found mass loss rates comparable to previous studies. To explain energy budget problem discussed in Drake et al. (2013), Odert et al. (2017) suggested then that probably the whole flare-CME association rate may shift to larger energies.Stellar flares are a subject of ongoing research going back to the first half of the last century where stellar flares have been detected using ground-based observations (Joy & Humason 1949; Luyten 1949, followed by numerous studies). With satellite missions such as the Microvariability and Oscillations of Stars Telescope (MOST), Convection, Rotation and planetary Transits (CoRoT), Kepler and now with the Transiting Exoplanet Survey Satellite (TESS) and in the near future also with the PLAnetary Transits and Oscillation of stars mission (PLATO) long-term photometric measurements were and will be accessible. This enabled statistical investigations of flares (see e.g. Balona 2015; Davenport 2016) and superflares ((E>1033 erg), see e.g. Maehara et al. 2012; Tu et al. 2020; Doyle et al. 2020; Tu et al. 2021; Okamoto et al. 2021). Flare-frequency distributions from TESS or Kepler are determined for more energetic flares, as usually such broadband photometric observations are insensitive to low energetic flares, as those simply leave no signature in a light-curve and are hidden in the noise.and are hidden in the noise. Stellar CMEs have been detected so far mainly on dMe stars (e.g. Houdebine et al. 1990; Guenther & Emerson 1997; Vida et al. 2016) using the method of Doppler shifted emission. This method uses the signature of plasma being ejected from a star. The signature, either appearing in absorption or emission is Doppler shifted by its projected velocity. This signature is often very pronounced in Balmer lines similarly to erupting filaments/prominences on the Sun. Optical spectroscopic monitoring programs to search for stellar CMEs using the method of Doppler shifted emission/absorption are often focused on dMe stars, as those are known to frequently flare and therefore also possibly may host CMEs. dG stars reveal also frequent flares if their X-ray luminosity is large, i.e. their activity level is high. However, for the detection of flares and CMEs, only stronger events, compared to dMe stars, may be detected, because of the higher continuum around Hα on those stars, or in other words a higher contrast is favorable for stellar CME detection using the method of Doppler-shifted emission/absorption in the Hα line.Only recently Namekata et al. (2021) presented the detection of a blue wing absorption in Hα during a superflare on the young solar analogue EK Dra, which the authors interpreted as an erupting filament. This event was simultaneously observed by two telescopes. Inoue et al. (2023) report on the detection of a high velocity blue-wing emission feature being interpreted by the authors as prominence eruption on the RS CVn system 1355 Ori, consisting of a K2-4 sub-giant and a G1 dwarf. Even more recently Namekata et al. (2024) focus again on EK Dra and present this time two prominence eruptions from which one has a projected bulk velocity being above the escape velocity of EK Dra and reveals a simultaneously observed candidate of coronal dimming. Using the method of Doppler shifted emission/absorption numerous candidate events have been found especially on dMe stars (e.g. Fuhrmeister et al. 2018; Vida et al. 2019). With this method only events with a projected bulk velocity being greater the stars’ escape velocity can be treated as eruptive events. It can be concluded that they are escaping from the star, as their true velocities can be even higher. But in numerous studies events with much smaller projected bulk velocities have been found which are much more difficult to interpret, as those may also originate from flaring plasma motions. To better interpret these spectral signatures investigating the Sun seen as a star may help. Instruments doing solar 2D spectroscopy are rare. In the 90ies of the last century MEES CCD provided Hα 2D spectroscopy of a cut-out of the solar-disk, in 2016 SMART/SDDI went into operation, doing full-disk multi-filter measurements resulting in a full-disk Hα profile, and only recently the Chinese Hα Solar Explorer (CHASE) providing full-disk Hα spectroscopy. MEES did Hα 2D Hα spectroscopy of solar cycles 22 and 23, so representing the past, whereas SMART/SDDI operated during the second half of cycle 24 and cycle 25 and CHASE beginning of cycle 25 up to now and hopefully also in the future. Spectroscopic Sun-as-a-star observations date back to the seventies of the last century (e.g. Livingston et al. 1981). Spatial integrated investigations of flares and erupting filaments have been presented by e.g. Den & Kornienko (1993); Ding et al. (2003); Ichimoto et al. (2017) and only recently progress has been made especially to understand Balmer line asymmetries related to erupting filaments/prominences (Namekata et al. 2021; Leitzinger et al. 2021; Namekata et al. 2022b; Otsu et al. 2022; Otsu & Asai 2024; Ma et al. 2024), as the Sun is the only star where we can actually see if a CME occurred in spatial and temporal vicinity to a filament/prominence eruption.