Holoea

Authors: Susanne M Hoffmann

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Holoea is a modern star name adopted by the International Astronomical Union in the IAU-Catalog of Star Names (IAU-CSN). Its origin is Hawaiian. It is the name of the star IRAS 05327+3404 (Vmag = 18.62) in constellation Auriga.

Concordance, Etymology, History

Young Stellar Object, the name is Hawaiian for "flowing gas", discovered by Magnier et al. (1996) with the James Clerk Maxwell Telescope at Mauna Kea, Hawaii.

Despite appearing close to the open star cluster M36 it is probably not a part of it. It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.

Morata et al. (2013):

The distance to the object is then somewhat uncertain, ranging from the 1.2 kpc adopted by Hron (1987)for M36 to the 1.6 kpc for S235 (Blitz et al. 1982). We adopt a distance of 1.2 kpc. IRAS 05327+3404 drives a powerful ionized outflow, seen in both CO (2–1) and optical spectra, with unusually high velocity (∼650 km s−1) for a low-mass star. The structure of IRAS 05327+3404 is not yet clear (see Magnier et al. 1999b). It could be a binary system with a central star of optical spectral type K2 III, which is probably an FU Orionis star similar to L1551 IRS 5 (Magnier et al. 1999b), and a still embedded young star powering the outflow. The young star was classified (Magnier et al. 1999a, 1999b) as a transitional YSO between Class I and Class II, because of its rising spectral energy distribution (SED) and molecular bipolar outflow as well as its visible central star and ionized outflow. The SED also shows the presence of large amounts of circumstellar material, which, according to optical and nearIR observations of the reflection nebula, seems to be arranged in a disk with a relatively wide central hole of ∼33◦ opening angle. The ionized flow, the CO outflow, and the hole are all roughly aligned and tilted by ∼45◦ to our line of sight (Magnier et al. 1996). Additionally, the brightness of the central star has increased >1.5 mag since the 1954 POSS plates. Magnier et al. (1999b) suggest that the source might be in the process of becoming exposed and hypothesized that the unusually wide SEDcouldbeduetotherelativeisolation of IRAS05327+3404, which allowed the formation of a large circumstellar disk with high angular momentum without being disrupted by external sources. Thus, this object seems to be a good candidate to study the transition from the Class I to the Class II phase in the evolution of YSOs. Subsequent 3.6 cm Very Large Array (VLA) observations by Anglada & Rodr´ıguez (2002) detected a source, named VLA 2, inside the error ellipsoid of IRAS 05327+3404, which coincides within ∼1arcsecof the optical position of Magnier et al. (1996). H2O maser emission surveys by Wouterloot et al. (1993), Codella et al. (1995), and Sunada et al. (2007) did not detect any maser emission near IRAS 05327+3404.

Mythology

no mythology

IAU Working Group on Star Names

The name was discussed and approved by the IAU WGSN in 2026, following a suggestion by the SIMBAD team.

Reference

• References (general)
• References (early modern)
• Ian Ridpath's website (Star Tales )