Tartalom
Képek
Kép feltöltése
DSS Images Other Images
Kapcsolódó cikkek
XMM-Newton study of the Serpens star-forming region
We analyze a XMM-Newton X-ray observation of the Serpens dark cloud witha total MOS-equivalent exposure time of 57 ksec. We find 45 individualX-ray sources. None of the class 0 protostars, only one of the class Iprotostars, and two of the flat-spectrum objects in the region aredetected in X-rays. The optically invisible flat-spectrum source EC 95,a very young intermediate mass object, is the strongest X-ray source inthe Serpens cloud. The analysis of its X-ray spectrum shows that thehydrogen column density towards EC 95 is considerably lower thanexpected from the extinction determined from near-IR spectroscopy andphotometry. Possible reasons for this inconsistency are discussed.
| Interstellar polarization in a molecular cloud in Serpens.
Not Available
| Interstellar extinction in the area of the Serpens cauda molecular cloud.
Not Available
| A preliminary compilation of DS-programme star positions
A catalog is presented of the double-star-program (DS-program) starpositions, listing right ascensions for 930 DSs and declinations for1225 DSs of the program. The positions were compiled from the observedvalues obtained between 1980 and 1987 with the meridian circles of sixUSSR observatories (the Moscow, Kazan', Kiev, Khar'kov, Odessa, andTashkent Observatories) and the Belgrade Observatory. The measurementsand the treatment of the observational material were performed using therelative method, and the FK-4 system stars were used as reference stars.
| Observations of the polarization of the radiation of R-association stars
A Ritchey-Chretien 1-m telescope was used to perform observations of thepolarization parameters of the radiation of stars in the reflectionnebulae in the regions of Cas, Per R1, Ser, and CMa R1. The connectionbetween the polarization vector and the structure of the nebulae isconsidered, and it is shown that the occurrence of polarization is dueboth to the absorption of the light of the stars and to scattering byelongated dust grains. The orientation of the grains is due to themagnetic field.
|
Új cikk hozzáadása
Kapcsolódó hivatkozások
- - (nincs kapcsolódó hivatkozás) -
Új link hozzáadása
Besorolás csoportokba:
|
Pozíciós és asztrometriai adatok
| Csillagkép: | Kígyó |
| Rektaszcenzió: | 18h29m57.66s |
| Deklináció: | +01°10'53.6" |
| Vizuális fényesség: | 8.474 |
| RA sajátmozgás: | -3.4 |
| Dec sajátmozgás: | -12.7 |
| B-T magnitude: | 8.657 |
| V-T magnitude: | 8.49 |
Katalógusok és elnevezések:
|
