Rho Ophiuchi

{{Short description|Multiple star system in the constellation Ophiuchus}}

{{about|the star|the dark cloud star forming region|Rho Ophiuchi cloud complex}}

{{Starbox begin

| name = ρ Ophiuchi

}}

{{Starbox image

|image=

{{Location mark

|image=Ophiuchus constellation map.svg|alt=|float=center|width=280

|label=|position=right

|mark=Red circle.svg|mark_width=10|mark_link=Rho Ophiuchi

|x=750|y=870

}}

|caption=Location of ρ Ophiuchi (circled red)

}}

{{Starbox observe

| epoch = J2000.0

| constell = Ophiuchus

| ra = {{RA|16|25|35.11766}}{{cite journal|title=Validation of the new Hipparcos reduction|author=van Leeuwen, F.|display-authors=etal|journal=Astronomy and Astrophysics|volume=474|issue=2|pages=653–664|date=2007|arxiv=0708.1752|bibcode=2007A&A...474..653V|doi=10.1051/0004-6361:20078357|s2cid=18759600}}

| dec = {{DEC|-23|26|49.8150}}

| appmag_v = 4.63{{Cite journal|bibcode=2002yCat.2237....0D|title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system|volume=2237|last1=Ducati|first1=J. R.|journal=VizieR Online Data Catalog|year=2002}}

}}

{{Starbox character

| component1 = ρ Oph AB

| class = B2/3V + B2V{{cite book|bibcode=1988mcts.book.....H|title=Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars. Volume 4, Declinations −26°.0 to −12°.0|last1=Houk|first1=N.|last2=Smith-Moore|first2=M.|year=1988}}

| b-v = +0.24{{cite journal|title=Catalogue of homogeneous data in the UBV photoelectric photometric system|date=1964|journal=Astronomy and Astrophysics Supplement Series|volume=34|pages=1–49|author=Nicolet, B.|bibcode=1978A&AS...34....1N}}

| u-b = −0.56

| variable =

}}

{{Starbox astrometry

| component1 = ρ Oph AB

| radial_v = {{val|−14.6|1.5}}

| prop_mo_ra = −5.53

| prop_mo_dec = −21.74

| pm_footnote =

| parallax = 7.19

| p_error = 0.13

| parallax_footnote =

| dist_pc = {{Val|138.2|3.6}}

| dist_ly = {{val|{{convert|138.2|pc|ly|disp=number}}|{{convert|3.6|pc|ly|disp=number}}|fmt=commas}}

| dist_footnote =

| absmag_v = {{val|-2.5|0.3}}{{cite journal|bibcode=2003AN....324..219W|doi=10.1002/asna.200310081|title=The total-to-selective extinction ratio determined from near IR photometry of OB stars|journal=Astronomische Nachrichten|volume=324|issue=3|pages=219–237|year=2003|last1=Wegner|first1=W.}}

}}

{{Starbox orbit

| primary = ρ Oph Aa

| name = ρ Oph Ab

| reference = {{Cite arXiv |last1=Klement |first1=R. |last2=Shultz |first2=M. E. |last3=Rivinius |first3=Th. |title=Spatially resolved centrifugal magnetosphere caught in motion around the secondary component of ρ Oph A |date=2025 |class=astro-ph.SR |eprint=2505.10038 }}

| period_unitless = {{Val|87.831|0.010}} days

| axis_unitless = {{Val|0.995|0.026|ul=AU}}

| eccentricity = {{Val|0.17931|0.00017}}

| inclination = {{val|71.348|0.020}}

| k1 = {{Val|55.5|3.6}}

| k2 = {{Val|65.7|3.6}}

| periarg = {{Val|4.80|0.24}}

| node = {{Val|303.385|0.034}}

| periastron = 60101.11 RJD

}}

{{Starbox orbit

| reference = {{cite journal|title=Orbits of Five Visual Binary Stars|author=Novaković, B.|journal=Baltic Astronomy|volume=16|pages=435–442|date=2007|bibcode=2007BaltA..16..435N|arxiv=0712.4242}}

| primary = ρ Oph A

| name = ρ Oph B

| period_unitless = {{val|2398|326|fmt=commas}} years

| axis = {{val|4.25|0.79}}

| eccentricity = {{val|0.675|0.322}}

| inclination = {{val|135.3|6.0}}

| node = {{val|77.5|13.5}}

| periastron = B {{val|2327|343}}

| periarg = {{val|226.1|15.3}}

}}

{{Starbox orbit

| reference =

| primary = ρ Oph D

| name = ρ Oph E

| period_unitless = {{val|675.5|32.5}} years

| axis = {{val|1.01|0.15}}

| eccentricity = {{val|0.707|0.112}}

| inclination = {{val|134.8|2.7}}

| node = {{val|152.7|4.6}}

| periastron = B {{val|2008.6|34.2}}

| periarg = {{val|260.4|1.1}}

}}

{{Starbox detail

| source =

| component1 = ρ Oph Aa

| mass = {{Val|9.21|0.79}}

| radius = {{val|4.2|0.3}}

| rotation = 1.205 days

| rotational_velocity = {{val|206|5}}

| luminosity = {{Val|4270|980|800|fmt=commas}}

| temperature = {{Val|23000|1000|fmt=commas}}

| gravity = {{Val|4.25|0.25}}

| age_myr = {{Val|15|6}}

| component2 = ρ Oph Ab

| mass2 = {{Val|7.79|0.70}}

| radius2 = {{Val|3.1|0.2}}

| luminosity2 = {{val|1000|400|290|fmt=commas}}

| temperature2 = {{val|19000|1000|fmt=commas}}

| gravity2 = {{Val|4.25|0.25}}

| age_myr2 = {{Val|15|6}}

| rotational_velocity2 = {{val|227|5}}

}}

{{Starbox detail | no_heading = y

| component1 = ρ Oph B

| mass = 8{{cite journal|doi=10.1093/mnras/sty2502|title=The dynamical evolution of multiple systems of trapezium type|year=2018|last1=Allen|first1=Christine|author1-link=Christine Allen (astronomer)|last2=Ruelas-Mayorga|first2=Alex|last3=Sánchez|first3=Leonardo J.|last4=Costero|first4=Rafael|journal=Monthly Notices of the Royal Astronomical Society|doi-access=free|arxiv=1809.03537}}

}}

{{Starbox detail | no_heading = y

| component1 = ρ Oph C

| mass = 5

}}

{{Starbox detail | no_heading = y

| component1 = ρ Oph D

| mass = 3.06

| component2 = ρ Oph E

| mass2 = 1.97

}}

{{Starbox catalog

| names = {{odlist|B=ρ Oph|F=5 Oph|WDS=J16256-2327}}

| component1=ρ Oph AB

| names1={{odlist|HIP=80473|CD=-23°12861}}

| component2=ρ Oph A

| names2={{odlist|HD=147933|HR=6112|SAO=184382}}

| component3=ρ Oph B

| names3={{odlist|HD=147934|HR=6113|SAO=184381}}

| component4=ρ Oph C

| names4={{odlist|HIP=80474|SAO=184383|CD=-23°12862}}

| component5=ρ Oph D/E

| names5={{odlist|HD=147888|HIP=80461|SAO=184377|CD=-23°12860}}

}}

{{Starbox reference

| Simbad=rho+Oph|sn=ρ Oph

| Simbad2=HD+147933|sn2=ρ Oph A

| Simbad3=HD+147934|sn3=ρ Oph B

| Simbad4=HD+147932|sn4=ρ Oph C

| Simbad5=HD+147888|sn5=ρ Oph D/E

}}

{{Starbox end}}

Rho Ophiuchi (ρ Ophiuchi) is a multiple star system in the constellation Ophiuchus. The central system has an apparent magnitude of 4.63. Based on the central system's parallax, it is located about 450 light-years distant. The other stars in the system are slightly farther away.{{clarify|reason=Slightly further away in distance from Earth or distance from the inner pair?|date=May 2025}}

System

File:Antares_and_Rho_Ophiuchi_by_Adam_Block.jpg (N is up): Antares is the bright star that looks yellow in this image, σ Scorpii is in the red nebula (Sh2-9), and the globular cluster M4 is in between. Rho Ophiuchi is the small group of stars in the blue nebulosity (IC 4604).]]

The central system is known as Rho Ophiuchi AB. It consists of three blue-colored subgiants or main-sequence stars, designated Rho Ophiuchi Aa, Ab and B, respectively. Rho Ophiuchi Aa-Ab is a spectroscopic binary with an orbital period of 88 days and an orbital period of 1.1 astronomical units.{{Cite arXiv |last1=Shultz |first1=M. E. |last2=Berry |first2=I. |last3=Bohlender |first3=D. |last4=Catanzaro |first4=G. |last5=Giarrusso |first5=M. |last6=Klement |first6=R. |last7=Labadie-Bartz |first7=J. |last8=Leone |first8=F. |last9=Leto |first9=P. |title=Discovery of the binary nature of the magnetospheric B-type star ρ Oph A |date=2025-05-12 |class=astro-ph.SR |eprint=2505.08007 }} Farther away is the B companion, a visual binary whose sky-projected distance from the inner pair appears to be 3.1″, corresponding to a separation of at least 344 AU.{{Cite journal|bibcode=2013ApJ...764L..10C|title=Cordiner, M. A., Fossey, S. J., Smith, A. M. and Sarre, P. J. 2013, ApJ, 764, L10|journal=The Astrophysical Journal Letters|volume=764|pages=L10|last1=Cordiner|first1=M. A.|last2=Fossey|first2=S. J.|last3=Smith|first3=A. M.|last4=Sarre|first4=P. J.|year=2013|issue=1|doi=10.1088/2041-8205/764/1/L10|arxiv = 1301.6167 |s2cid=119204101|url=https://zenodo.org/record/897951}} However, the actual separation is larger, and the two take about 2,400 years to complete an orbit. The two stars dominate the radiation field around the Rho Ophiuchi cloud complex.{{cite journal|doi=10.1002/asna.201713457|title=Detection of a centrifugal magnetosphere in one of the most massive stars in the ρ Oph star-forming cloud|year=2018|last1=Hubrig|first1=S.|last2=Schöller|first2=M.|last3=Järvinen|first3=S. P.|last4=Küker|first4=M.|last5=Kholtygin|first5=A. F.|last6=Steinbrunner|first6=P.|journal=Astronomische Nachrichten|volume=339|issue=1|pages=72–77|arxiv=1712.05939|bibcode=2018AN....339...72H|s2cid=119084902}}

Rho Ophiuchi A emits X-rays, and exhibits strong variability in emission over periods of about 1.2 days, corresponding to its rotation period. The X-ray variability is due to the strong magnetic field of the secondary companion, Rho Ophiuchi Ab, whose dipole strength is 4 kG.{{cite journal|doi=10.1051/0004-6361/201630070|title=The early B-type star Rho Ophiuchi a is an X-ray lighthouse|year=2017|last1=Pillitteri|first1=Ignazio|last2=Wolk|first2=Scott J.|last3=Reale|first3=Fabio|last4=Oskinova|first4=Lida|journal=Astronomy & Astrophysics|volume=602|pages=A92|arxiv=1703.04686|bibcode=2017A&A...602A..92P|s2cid=119431278}}

Several other stars are located close to Rho Ophiuchi AB. HD 147932 is located 2.5 arcminutes away (at least 17,000 AU), and is known as Rho Ophiuchi C. HD 147888 is located 2.82 arcminutes away (at least 19,000 AU), and is known as Rho Ophiuchi DE. Stars C and D are both B-type main-sequence stars, and D itself is another binary with an orbital period of around 680 years.

Cloud complex

{{main|Rho Ophiuchi cloud complex}}

Rho Ophiuchi is the namesake of the Rho Ophiuchi cloud complex. It is a nebula of gas and dust, which the Rho Ophiuchi system is embedded in. It is one of the easiest star forming regions to observe, as it is one of the nearest, and it is visible from both hemispheres.{{cite journal|bibcode=2008hsf2.book..351W|arxiv=0811.0005|title=Star Formation in the ρ Ophiuchi Molecular Cloud|author1=Wilking, B. A.|author2=Gagné, M.|author3=Allen, L. E.|author3-link=Lori Allen (astronomer)|journal=Handbook of Star Forming Regions|date=2008}}

The interstellar extinction (AV) of Rho Ophiuchi is measured to be 1.45 magnitudes, meaning the dust and gas in front of Rho Ophiuchi absorbs light from the system, making it appear 1.45 magnitudes dimmer than it would be if there were no dust or gas.{{cite journal|title=The mass ratio distribution of B-type visual binaries in the Sco OB2 association|author1=Shatsky, N.|author2=Tokovinin, A.|journal=Astronomy and Astrophysics|volume=382|pages=92–103|date=2002|bibcode=2002A&A...382...92S|doi=10.1051/0004-6361:20011542|arxiv=astro-ph/0109456|s2cid=16697655}} Additionally, gas and dust also scatters more higher-frequency light, leaving the light appearing more reddish. The interstellar reddening (EB−V) of Rho Ophiuchi has been measured to be 0.47 magnitudes.

{{clear left}}

References