Mass and Kinetic Energy of the Homunculus Nebula around η Carinae

By N. Smith, R. Gehrz, P. Hinz, W. Hoffmann, J. Hora, Eric Mamajek, M. Meyer. 2003

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In Astronomy and Astrophysics

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Luminous blue variables are antisocial: their isolation implies that they are kicked mass gainers in binary evolution (2014, background): “As seen in the case of η Car, these eruptions can eject 10-20 M⊙ in a single event (Smith et al. 2003a).”
SPECTRAL EVOLUTION OF THE EXTRAORDINARY TYPE IIn SUPERNOVA 2006gy (2009, background): “The most important of these are the total ejected mass of 10–20 M⊙ (Smith et al. 2003), launched at speeds of 100–600 km s−1 with a Hubble-like velocity law indicating a brief event (Smith 2006a), and the H-rich composition.”
Dust Formation and He II λ4686 Emission in the Dense Shell of the Peculiar Type Ib Supernova 2006jc (2007, background): “Normal LBV eruptions are known to be copious dust producers (e.g., Smith et al. 2003), so we cannot exclude the possibility of considerable dust in the CSM around SN 2006jc.”
ON THE MAXIMUM MASS OF STELLAR BLACK HOLES (2009, background): “For the extreme case of η Carinae the amount of mass lost has been suggested to be substantial (∼ 10 M⊙; Smith et al. 2003).”
A Porosity-Length Formalism for Photon-Tiring-limited Mass Loss from Stars above the Eddington Limit (2004, background): “Moreover, there is evidence, from both ground-based interferometric observations (van Boekel et al. 2003) and from HST slit-spectra (Smith et al. 2003), the present-day wind of η Carinae is also bipolar about the same symmetry axis as the Homunculus.”
Shell-shocked Diffusion Model for the Light Curve of SN 2006gy (2007, result): “This would have been analogous to events observed in very massive progenitor stars like η Carinae, which ejected 10-15 M⊙ in about a decade (Smith & Owocki 2006; Smith et al. 2003).”
Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “The best studied example is the Galactic object η Carinae, providing us with its historically observed light curve (Smith & Frew 2011), as well as its complex ejecta that contain 10-20 M⊙ and ∼1050 ergs of kinetic energy (Smith 2006, Smith et al. 2003).”
SN 2006gy: Discovery of the Most Luminous Supernova Ever Recorded, Powered by the Death of an Extremely Massive Star like η Carinae (2006, background): “We do not know the electron density in the nebula around SN 2006gy, but values of 105–106 cm 3 are the highest densities typically seen in young LBV nebulae like the one around Carinae (Smith 2006).”
The Unprecedented Third Outburst of SN 2009ip: A Luminous Blue Variable Becomes a Supernova (2012, result): “This is in contrast with more massive LBV ejection nebulae, such as η Car’s Homunculus or the Pistol nebula, both of which have masses of ∼ 10M⊙ (Smith et al. 2003; Figer et al. 1999).”
Luminous blue variable eruptions and related transients: diversity of progenitors and outburst properties (2010, background): “Following another smaller eruption in ∼1890, the star is apparently still slowly recovering from the upheaval of its 19th century eruptions (e.g., Smith et al. 2003a; Davidson et al. 2005).”
Physical Properties of Wolf-Rayet Stars (2006, background): “Giant eruptions are believed to play a major role in the evolution of very massive stars via the removal of their hydrogen-rich envelope (Davidson & Humphreys 1997; Smith et al. 2003).”
The Structure of the Homunculus. I. Shape and Latitude Dependence from H2 and [Fe II] Velocity Maps of η Carinae (2006, methodology): “This is because the H2 emission traces the cool and dense outer skin of theHomunculus, which thermal-IR observations indicate contains the majority of the nebula’s mass and kinetic energy (Smith et al. 2003b).”
On the Role of Continuum-driven Eruptions in the Evolution of Very Massive Stars and Population III Stars (2006, background): “…mass leave no room for such substantial mass loss if there is an upper limit of 150 M⊙ to the initial masses of stars (Figer 2005; Kroups 2005). in 1890 (Smith 2005; Ishibashi et al. 2003), and it may suffer smaller ejections every 5.5 years (Davidson 1999; Smith et al. 2003a; Martin et al. 2006).”
Pulsational Pair-instability Supernovae (2016, background): “Smith et al. (2003) further estimates that this matter carries a kinetic energy of 1049.6 - 1050 erg. Smith (2008) and Smith (2013) have made a compelling case that the production of the Great Eruption required an explosive event, not just a strong wind.”
Mass loss from hot massive stars (2008, background): “For instance, the giant eruption ofη Car with a cumulative loss of∼10 M⊙ between 1840 and 1860 (Smith et al 2003b) which resulted in the Homunculus nebula corresponds to Ṁ ≈ 0.1-0.5M⊙yr−1, which is a factor of 1000 larger than that expected from a line-driven wind at that luminosity.”
A Survey About Nothing: Monitoring a Million Supergiants for Failed Supernovae (2008, background): “Spectacular outbursts such as that of η Carina in the 19th century (Smith et al. 2003; Morse et al. 2001) and P Cygni (Walborn 1976; Smith & Hartigan 2006) around 1600 CE should be recognizable by a characteristic brightening, reddening, and then decay back to quiescence.”
Ancient eruptions of η Carinae: a tale written in proper motions (2016, background): “During this Great Eruption, η Car ejected an estimated 10–15 M⊙ into the wellknown bipolar Homunculus nebula (Smith et al. 2003).”
DISCOVERY OF PRECURSOR LUMINOUS BLUE VARIABLE OUTBURSTS IN TWO RECENT OPTICAL TRANSIENTS: THE FITFULLY VARIABLE MISSING LINKS UGC 2773-OT AND SN 2009ip (2009, background): “…nor giant LBV eruptions have a theoretical explanation, although they are suspected to be the result of luminous stars flirting with an opacity-modified Eddington limit and subsequent runaway mass loss (e.g., Smith & Owocki 2006; Humphreys & Davidson 1994; Smith et al. 2003; Owocki et al. 2004).”
The evolution of hierarchical triple star-systems (2016, background): “10erg (Smith et al., 2003) and comes close to that of normal supernovae.”
Massive stars exploding in a He-rich circumstellar medium. I. Type Ibn (SN 2006jc-like) events (2008, background): “These outbursts are likely accompanied by an ejection of∼10 M⊙ of material (Smith et al. 2003), which is uncomfortably large to be consistent with an evolved WR progenitor.”