Talk:VV Cephei

VV Cephei

W Cephei is by far I know the bigest star in the Unerverse there might be bigger stars that havnt been discovred —Preceding unsigned comment added by 81.156.32.168 (talk) 13:47, 22 February 2008 (UTC)

The size of this monster is completely incomprehensible to me. My head hurts just trying to imagine it. Primal Eighties (talk) 23:42, 4 August 2008 (UTC)

How big of a tatonka size telescope do you need for this? —Preceding unsigned comment added by Kingkong77 (talk • contribs) 14:30, 7 October 2008 (UTC)

W Cephei is not VV Cephei. — Preceding unsigned comment added by Red Planet X (Hercolubus) (talk • contribs) 15:48, 3 September 2016 (UTC)

Location

Doesn't seem to be right that puts me right outside of hercules, not cepheus--Vennificus (talk) 01:24, 15 March 2010 (UTC)

Red circle indicates location in Cepheus

The location checks out correct according to my printed Norton's Star Atlas: it lies between iota and alhpa Cepheus. I have added this location map. -84user (talk) 19:17, 16 March 2010 (UTC)

Pronunciation

Is this "Vee Vee" Cephei, or "Five Five", or something else? Or is it something in Greek that hadn't occurred to me? :o) - 94.194.113.136 (talk) 16:25, 16 May 2012 (UTC) (just a passer-by)

It's vee vee, it's from the Bayer designation, which initially used Latin letters after the 24 Greek ones had expired, but this only survived mainly in designations for variable stars, which always begin with a letter from R to Z. - filelakeshoe 20:03, 16 May 2012 (UTC)

Image submitted for deletion

An image on this page has been submitted for deletion from Commons. See c:Commons:Deletion requests/File:VVCephei1.png Lithopsian (talk) 16:11, 29 November 2016 (UTC)

How much is "dramatically lower"?

From the "Properties" section (emphasis not in original):

"The traditional model, from the spectroscopically derived orbit, has the masses of both stars around 20 M☉, which is typical for a luminous red supergiant and an early A main sequence star.[7] An alternative model has been proposed based on the unexpected timing of the 1997 eclipse. Assuming that the change is due to mass transfer altering the orbit, dramatically lower mass values are required. In this model, the primary is a 18.2 M☉ AGB star and the secondary is an 18.4 M☉ B star."

Depending on the meaning of "around", 18.2 and 18.4 could be well within the error anticipated. Unless it means "19 to 21", where it would be a near miss, or "20 rounded to the nearest integer", where it would be definitely on the low side. But even if it is, 18.2 and 18.4 would be 9% and 8% low, nothing I'd call "dramatically."

If an 8% discrepancy is unusual, I'd recommend adding a few words why it is (not exactly WEASEL wording, but a similar, less malicious issue). - ¡Ouch! (^{hurt me} / _{more pain}) 15:11, 6 July 2017 (UTC)

Good catch. They got changed at some point. I've changed them back to what the references says. Lithopsian (talk) 15:22, 6 July 2017 (UTC)

Cool. Now what to put into the infobox? I'd think we should put a note there, say a [note 1] which reads

"according to high-mass model (see "Properties" section)"

At any rate, good work. I ran into that other infobox earlier today, which I repaired on my own... ;) - ¡Ouch! (^{hurt me} / _{more pain}) 16:26, 6 July 2017 (UTC)

A Commons file used on this page has been nominated for deletion

The following Wikimedia Commons file used on this page has been nominated for deletion:

• Comparison of planets and stars (2017 update).png

Participate in the deletion discussion at the nomination page. Community Tech bot (talk) 07:52, 28 June 2018 (UTC)

New estimate for VV Cephei A

According to Nussun05, Messineo & Brown 2019 listed VV Cephei A as 388 R_☉ based on the luminosity and temperature though I can't find luminosity and temperature of the listed stars in any tables or pages in the given citation. Should we use it? 2A01:E0A:47A:F100:D025:C6CB:707E:5CDA (talk) 07:44, 23 May 2020 (UTC)

The data is online at VizieR. It assumes the Gaia DR2 distance of 599 pc, which is barely a third of the consensus value of 1,500 pc. Hence a much lower luminosity of 24,000 L_☉ and the smaller radius. The radius value should be treated with caution since it is based on treating the whole system as a single star. Although the parallax has quite a large formal error, as well as no corrections for being a binary, it is consistent with the Hipparcos parallax which has been ignored or dismissed by most authors until now. Surely at least worth a mention in the text even if it isn't yet the accepted value. Lithopsian (talk) 13:09, 23 May 2020 (UTC)

Contradiction

Recent research contradicts the beginning of this article, where it states that mass transfer occurs via Roche lobe overflow. Whmbkx (talk) 01:44, 21 November 2020 (UTC)

Could you please provide a link to said research? Primefac (talk) 12:43, 21 November 2020 (UTC)

How reliable is Stassun, K. G.; et al. (2019)?

Should this value really be used in the starbox? It is based on Gaia Data Release 2 data, and has a massive significance of astrometric excess noise. Pollman, E.; et al. (2018) is a study solely based on VV Cephei itself. It should be used over 516 R_☉. Faren29 (talk) 22:54, 25 December 2020 (UTC)

Parallaxes from Hipparcos, DR2, and EDR3, are all similar, around a milli-arcsecond. High astrometric noise indicates a possible issue, not that the value is wrong. High astrometric noise is expected for a binary, non-stellar object such as VV Cep, and the parallax may still have some merit. The "classical" distance from other methods is around 1.5 kpc, but also highly uncertain. Pollman et al. adds nothing to the equation, it is just repeating earlier results (eg. Bauer et al., 2008) and not deriving new ones. "~1,000" should probably be dropped from the starbox and replaced with something specific such as 1,050 R_☉ from Bauer et al. Lithopsian (talk) 16:05, 27 December 2020 (UTC)

1,050 R_☉ from Hagen Bauer, Wendy; et al. (2008) seems trustworthy, but Hopkins, Jeffrey L.; et al. (2015) also references many radii for VV Cephei A. This includes: 1,000 R_☉, which is most likely the same case you described for Pollman, Ernst; et al (2019), 1,015 R_☉, from Bennett, Philip D. (2007), 1,600 R_☉, from Wright, K. O. (1977) and Hack, M.; et al. (1992), and 1,800 R_☉, from Hutchings, J. B. and Wright, K. O. (1971). Aside from the trusted value of 1,050 R_☉, are there any values that could potentially be used in the starbox in Hopkins, Jeffrey L.; et al. (2015)? Faren29 (talk) 19:10, 27 December 2020 (UTC)

There is a short section about the distance. You could expand that and mention the various estimates and the inconsistencies between the parallaxes (600-1000 pc) and distances from methods like the orbit and eclipses (1,500+ pc). I wouldn't put anything from last century in the starbox. Then decide which of the radius values comes out as most reliable for the starbox. Lithopsian (talk) 14:36, 28 December 2020 (UTC)

Inconsistency in starbox parallax and distance

The values for parallax and distance in the starbox are mutually exclusive. The given parallax of 1.33±0.20 mas corresponds to between 654 and 885 pc, approximately half the stated 1500 pc.

The reference for the parallax (Van Leeuwen, 2007) is a paper which applies new methodology for processing the Hipparcos to improve its overall accuracy. It deals with the data set as a whole; the only places where it refers to the parallax of specific stars (for purpose of illustration) are in Table 1 on page 7 (stars HIP 70 and HIP 71) and Table 2 on page 10 (ten stars, 5 with names). None of the mentioned stars appear to be VV Cephei.

Please change

{{Starbox astrometry | parallax=1.33 | p_error=0.20 | parallax_footnote=<ref name=hipparcos/>

to

{{Starbox astrometry | parallax=1.33 | p_error=0.20 | parallax_footnote=<ref name=hipparcos/>{{Failed verification|date=June 2021}}

98.110.77.253 (talk) 02:14, 26 June 2021 (UTC)

 Done, and thank you for the good catch! We won't change the figures just yet; however, we will continue to dig. P.I. Ellsworth  ed. ^put'r there 15:31, 30 June 2021 (UTC)