3 Vulpeculae

{{Short description|Star in the constellation Vulpecula}}

{{Starbox begin

| name = 3 Vulpeculae

}}

{{Starbox image

| image = 250px

| caption = A light curve for V377 Vulpeculae, plotted from TESS data

}}

{{Starbox observe

| epoch = J2000.0

| constell = Vulpecula

| ra = {{RA|19|22|50.8856}}

| dec = {{DEC|+26|15|44.667}}

| appmag_v = 5.18

}}

{{Starbox character

| class = B6 III{{cite journal|bibcode=1977A&AS...30...71C|title=Spectral classification from the ultraviolet line features of S2/68 spectra. II - Late B-type stars|journal=Astronomy and Astrophysics Supplement Series|volume=30|pages=71|last1=Cucchiaro|first1=A.|last2=Macau-Hercot|first2=D.|last3=Jaschek|first3=M.|last4=Jaschek|first4=C.|year=1977}}

| r-i =

| v-r =

| b-v = {{Val|−0.119|0.001}}{{cite journal

| title=XHIP: An extended hipparcos compilation

| last1=Anderson | first1=E. | last2=Francis | first2=Ch.

| journal=Astronomy Letters | arxiv=1108.4971

| volume=38 | issue=5 | pages=331 | year=2012

| bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015 | s2cid=119257644 }}

| u-b =

| variable = SPB{{cite journal

| display-authors=1 | last1=Samus | first1=N. N.

| last2=Kazarovets | first2=E. V. | last3=Durlevich | first3=O. V.

| last4=Kireeva | first4=N. N. | last5=Pastukhova | first5=E. N.

| title=General Catalogue of Variable Stars

| version=5.1 | journal=Astronomy Reports

| year=2017 | volume=61 | issue=1 | pages=80–88

| doi=10.1134/S1063772917010085 | bibcode=2017ARep...61...80S | s2cid=125853869 }}

}}

{{Starbox astrometry

| radial_v = {{Val|−14.1|1.1}}

| prop_mo_ra = {{val|0.922|(124)}}

| prop_mo_dec = {{val|−10.270|(163)}}

| pm_footnote =

| parallax = 8.9071

| p_error = 0.1685

| parallax_footnote =

| absmag_v = −0.17

}}

{{Starbox orbit

| reference =

| period_unitless = 367.7

| eccentricity = 0.15

| k1 = 6.8

}}

{{Starbox detail

| component1 = A

| mass = 4.16

| radius =

| luminosity = {{Val|286|64|52}}{{cite journal

| title=Constraints on stellar parameters of the slowly pulsating B star HD 182255 from complex asteroseismology

| last1=Walczak | first1=P. | last2=Szewczuk | first2=W.

| last3=Daszyńska-Daszkiewicz | first3=J. | display-authors=1

| journal=Astronomische Nachrichten

| volume=333 | issue=10 | page=1065 | date=December 2012

| doi=10.1002/asna.201211824 | bibcode=2012AN....333.1065W

| arxiv=1212.4643 | s2cid=116926922 }}

| gravity = 4.30

| temperature = 14,343

| metal_fe =

| rotational_velocity = 15.5{{cite journal

| title=Stars with discrepant v sin i as derived from the Ca II λ3933 Å and Mg II λ4481 Å lines. V. HD 182255 and HD 214923—SPB stars in binary systems

| last1=Zverko | first1=J. | last2=Romanyuk | first2=I.

| last3=Iliev | first3=I. | last4=Kudryavtsev | first4=D.

| last5=Stateva | first5=I. | last6=Semenko | first6=E.

| journal=Astrophysical Bulletin

| volume=71 | issue=2 | pages=199–207 | date=April 2016

| doi=10.1134/S1990341316020073 | bibcode=2016AstBu..71..199Z | s2cid=124871780 }}

| component2 = B

| mass2 = 0.6 - 1.1

| age_myr2 = 25

}}

{{Starbox catalog

| names = {{odlist | V=V377 Vulpeculae | F=3 Vul | BD=+25°3811 | HD=182255 | HIP=95260 | HR=7358 | SAO=87136 | GC=26748 }}{{cite simbad | title=3 Vul | access-date=2019-03-13 }}

}}

{{Starbox reference

| Simbad = HD+182255

}}

{{Starbox end}}

3 Vulpeculae (abbreviated 3 Vul) is a binary star system in the northern constellation of Vulpecula, located around 366 light years away from the Sun. 3 Vulpeculae is its Flamsteed designation. It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.18.

3 Vul has been nicknamed "the Observer's Nightmare" (or its Latin free translation, "Spectatori Error Inextricabilis") by some astronomers{{cite web

|title=3 Vul

|first=Jim|last=Kaler

|url=http://stars.astro.illinois.edu/sow/3vul.html

|access-date=2016-08-09}}{{cite journal

| last1 = Dukes

| first1 = Robert

| last2 = Kubinec

| first2 = William

| last3 = Kubinec

| first3 = Angela

| last4 = Adelman

| first4 = Saul

| date = 2003

| title = A Photometric and Spectroscopic Study of 3 Vulpeculae: An Observer's Nightmare

| journal = The Astronomical Journal

| volume = 126

| issue = 1

| pages = 370

| doi = 10.1086/375463

|bibcode = 2003AJ....126..370D | doi-access= free

}} because it is difficult to study as its orbital period is close to a year, and additionally it is pulsating with a period close to a day.

From a twenty-year spectroscopic study, Hube and Aikman established a 367-day orbital period, and noted the presence of non-radial pulsations in the primary star. From sparse photometry, the authors also established the star's light variability. They suggested that the primary is a member of the 53 Persei class of variable stars.{{cite journal |title=3 Vulpeculae: A non-radial pulsator in a one-year binary system |journal=Publications of the Astronomical Society of the Pacific |date=1991 |volume=103 |issue=659 |pages=49–62 |doi=10.1086/132794 |bibcode=1991PASP..103...49H | doi-access= free|last1=Hube |first1=Douglas P. |last2=Aikman |first2=G. C. L. }} Such stars are now collectively known by the term slowly pulsating B-type stars. Its photometric variation led to a variable star designation, as V377 Vulpeculae, but the non-reproducibility of the light curve made determination of the pulsation period elusive.

Continuous monitoring of the star by the Transiting Exoplanet Survey Satellite has revealed a beat-period phenomenon in the light curve, which causes the luminosity variations to fluctuate in amplitude. The pulsations are non-radial, that is, the star's photosphere varies in shape rather than volume; different parts of the star are expanding and contracting simultaneously. These gravity waves, or g-mode waves, can be indicative of the interior structure of the star.{{citation needed|date=December 2022}}

The primary member, designated component A, is a most likely a B-type main-sequence star with a stellar classification of B6 III. The star has 4.16 times the mass of the Sun and is radiating 286 times the Sun's luminosity from its photosphere at an effective temperature of 14,343 K. The secondary has an estimated 0.6–1.1 solar masses.