title: ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ ÑÐ¿Ð¾ÐºÐ¾Ð¹Ð½ÑÑ Ð¼Ð°Ð»Ð¾Ð¼Ð°ÑÑÐ¸Ð²Ð½ÑÑ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¸Ñ Ð´Ð²Ð¾Ð¹Ð½ÑÑ Ð·Ð²ÐµÐ·Ð´Ð½ÑÑ ÑÐ¸ÑÑÐµÐ¼ X5 Ð¸ X7 Ð² ÑÐ°ÑÐ¾Ð²Ð¾Ð¼ ÑÐºÐ¾Ð¿Ð»ÐµÐ½Ð¸Ð¸ 47 Tuc
title: Ð²ÑÐ¿ÑÑÐºÐ½Ð°Ñ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÐ°
titleType: Subtitle
title: Studies of the quiescent low-mass X-ray binaries X5 and X7 in the globular cluster 47 Tucanae
Creators: name: Ð¦Ð²ÐµÑÐºÐ¾Ð², ÐÐ²Ð°Ð½
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2021
Subjects: ÑÐ¿Ð¾ÐºÐ¾Ð¹Ð½ÑÐµ Ð¼Ð°Ð»Ð¾Ð¼Ð°ÑÑÐ¸Ð²Ð½ÑÐµ Ð´Ð²Ð¾Ð¹Ð½ÑÐµ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¸Ðµ ÑÐ¸ÑÑÐµÐ¼Ñ
Ð½ÐµÐ¹ÑÑÐ¾Ð½Ð½ÑÐµ Ð·Ð²ÐµÐ·Ð´Ñ
ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¸Ðµ Ð½Ð¾Ð²ÑÐµ
Ð´Ð¸Ð°Ð³ÑÐ°Ð¼Ð¼Ð° ÑÐ²ÐµÑ-Ð·Ð²ÐµÐ·Ð´Ð½Ð°Ñ Ð²ÐµÐ»Ð¸ÑÐ¸Ð½Ð°
ngc 104
tuc 47
ÑÐµÑÐ½ÑÐµ Ð´Ð²Ð¾Ð¹Ð½ÑÐµ ÑÐ¸ÑÑÐµÐ¼Ñ
iraf
gemini
ÐºÐ¾ÑÐ¼Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐµÐ»ÐµÑÐºÐ¾Ð¿ Ñ Ð°Ð±Ð±Ð»Ð°
ÑÐ¾ÑÐ¾Ð¼ÐµÑÑÐ¸Ñ
Ð±ÐµÐ»ÑÐµ ÐºÐ°ÑÐ»Ð¸ÐºÐ¸
quiescent low-mass x-ray binaries systems
neutron star
x-ray novae
colour magnitude diagram (cmd)
globular cluster
contact binary
hubble space telescope
photometry
white dwarfs

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ ÑÐ¿Ð¾ÐºÐ¾Ð¹Ð½ÑÑ Ð¼Ð°Ð»Ð¾Ð¼Ð°ÑÑÐ¸Ð²Ð½ÑÑ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¸Ñ Ð´Ð²Ð¾Ð¹Ð½ÑÑ Ð·Ð²ÐµÐ·Ð´Ð½ÑÑ ÑÐ¸ÑÑÐµÐ¼ X5 Ð¸ X7 Ð² ÑÐ°ÑÐ¾Ð²Ð¾Ð¼ ÑÐºÐ¾Ð¿Ð»ÐµÐ½Ð¸Ð¸ 47 Tuc. ÐÐ½Ð°Ð»Ð¸Ð· Ð´Ð°Ð½Ð½ÑÑ Ð¿ÑÐ¾Ð²ÐµÐ´ÐµÐ½, Ð¾ÑÐ½Ð¾Ð²ÑÐ²Ð°ÑÑÑ Ð½Ð° Ð½Ð°ÑÑÐ½ÑÑ Ð´Ð°Ð½Ð½ÑÑ Ð¸Ð·ÑÑÐ°ÐµÐ¼Ð¾Ð³Ð¾ ÑÐ°ÑÐ¾Ð²Ð¾Â­Ð³Ð¾ ÑÐºÐ¾Ð¿Ð»ÐµÐ½Ð¸Ñ, Ð½Ð°Ð±Ð»ÑÐ´Ð°ÐµÐ¼Ð¾Ð³Ð¾ Ð´Ð²ÑÐ¼Ñ Ð¾Ð±ÑÐµÑÐ²Ð°ÑÐ¾ÑÐ¸ÑÐ¼Ð¸ Ð² ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ ÑÐºÑÐ¿Ð¾Ð·Ð¸ÑÐ¸ÑÑ Ð¸ ÑÐ¸Ð»ÑÑÑÐ°Ñ: Gemini GSAOI â ÑÐµÑÐ¸Ñ ÑÐ½Ð¸Ð¼ÐºÐ¾Ð² Ð² Ð¸Ð½ÑÑÐ°ÐºÑÐ°ÑÐ½Ð¾Ð¼ ÑÐ¿ÐµÐºÑÑÐ°Ð»ÑÐ½Ð¾Ð¼ Ð´Ð¸Ð°Ð¿Ð°Ð·Ð¾Ð½Ðµ (ÑÐ¸Ð»ÑÑÑÑ Ks Ð¸ J, ÑÐºÑÐ¿Ð¾Ð·Ð¸ÑÐ¸Ð¸ 30 Ð¸ 60 ÑÐµÐºÑÐ½Ð´); ÐÐ¾ÑÐ¼Ð¸ÑÐµÑÐºÐ¸Ð¹ Ð¢ÐµÐ»ÐµÂ­ ÑÐºÐ¾Ð¿ Ð¸Ð¼. Ð¥Ð°Ð±Ð±Ð»Ð° (HST) â ÑÐµÑÐ¸Ñ ÑÐ½Ð¸Ð¼ÐºÐ¾Ð² Ð² Ð¾Ð¿ÑÐ¸ÑÐµÑÐºÐ¾Ð¹ ÑÐ°ÑÑÐ¸ ÑÐ¿ÐµÐºÑÑÐ° (ÑÐ¸Ð»ÑÑÑÑ F275W, F336W, F438W, F555W, F606W, F814W, Ð² Ð²ÑÑÐ¾ÐºÐ¾Ð¹ ÑÐºÑÐ¿Ð¾Ð·Ð¸ÑÐ¸Ð¸ Ð¿Ð¾ÑÑÐ´ÐºÐ° 720 ÑÐµÐºÑÐ½Ð´). ÐÐ°Ð¶Ð´Ð°Ñ Ð¸Ð· Ð½Ð°Ð±Ð»ÑÐ´Ð°ÐµÐ¼ÑÑ ÑÐ¸ÑÑÐµÐ¼ Ð½Ð°Ð½ÐµÑÐµÐ½Ð° Ð½Ð° Ð´Ð¸Ð°Ð³ÑÐ°Ð¼Ð¼Ñ ÐÐµÑÑÑÐ¿ÑÑÐ½Ð³Ð°-Ð Ð°ÑÑÐµÐ»Ð°, Ð¿Ð¾ÑÑÑÐ¾ÐµÐ½Ð½ÑÑ Ð´Ð»Ñ ÑÐ°ÑÐ¾Ð²Ð¾Ð³Ð¾ ÑÐºÐ¾Ð¿Ð»ÐµÐ½Ð¸Ñ NGC 104 Ð² Ð´Ð²ÑÑ Ð½Ð°Ð±Ð¾ÑÐ°Ñ ÑÐ¸Ð»ÑÑÑÐ¾Ð²: F606W, F814W (Ð¾ÑÐ½Ð¾Ð²ÑÐ²Ð°ÑÑÑ Ð½Ð° Ð´Ð°Ð½Ð½ÑÑ Ð¿ÑÐ¾ÐµÐºÑÐ° HUGS) Ð¸ F555W, Ks (Ð¿ÑÐ¸ Ð¸ÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð½Ð¸Ð¸ ÑÐ¾Ð²Ð¾ÐºÑÐ¿Ð½ÑÑ Ð´Ð°Ð½Ð½ÑÑ Ð´Ð²ÑÑ Ð¾Ð±ÑÐµÑÐ²Ð°ÑÐ¾ÑÐ¸Ð¹). ÐÐ¾ Ð¿Ð¾Ð»ÑÑÐµÐ½Ð½ÑÐ¼ Ð·Ð°Ð²Ð¸ÑÐ¸Ð¼Ð¾ÑÑÑÐ¼ ÑÐ´ÐµÐ»Ð°Ð½ Ð²ÑÐ²Ð¾Ð´ Ð¾ Ð¿ÑÐ¸Ð½Ð°Ð´Ð»ÐµÐ¶Ð½Ð¾ÑÑÐ¸ Ð²ÑÐ¾ÑÐ¸ÑÐ½Ð¾Ð³Ð¾ Ð¼Ð°Ð»Ð¾Ð¼Ð°ÑÑÐ¸Ð²Ð½Ð¾Ð³Ð¾ ÐºÐ¾Ð¼Ð¿Ð°Ð½ÑÐ¾Ð½Ð° Ð´Ð²ÑÑ ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ ÑÐ¸ÑÑÐµÐ¼ Ðº Ð·Ð²ÐµÐ·Ð´Ð°Ð¼ Ð³Ð»Ð°Ð²Ð½Ð¾Ð¹ Ð¿Ð¾ÑÐ»ÐµÐ´Ð¾Ð²Ð°ÑÐµÐ»ÑÐ½Ð¾ÑÑÐ¸ (MSS). ÐÐ¾Ð»Ð¾Ð¶ÐµÐ½Ð¸Ðµ Ð¾Ð¿ÑÐ¸ÑÐµÑÐºÐ¾Ð³Ð¾ ÐºÐ¾Ð¼Ð¿Ð°Ð½ÑÐ¾Ð½Ð° ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð³Ð¾ Ð¸ÑÑÐ¾ÑÐ½Ð¸ÐºÐ° Ñ5 Ð½Ð° Ð´Ð¸Ð°Â­Ð³ÑÐ°Ð¼Ð¼Ðµ ÐÐµÑÑÑÐ¿ÑÑÐ½Ð³Ð°-Ð Ð°ÑÑÐµÐ»Ð° Ð¿Ð¾Ð·Ð²Ð¾Ð»Ð¸Ð»Ð¾ Ð¾Ð¿ÑÐµÐ´ÐµÐ»Ð¸ÑÑ ÐµÐ³Ð¾ ÑÐ¿ÐµÐºÑÑÐ°Ð»ÑÐ½ÑÐ¹ ÐºÐ»Ð°ÑÑ â ÐºÐ°ÑÐ»Ð¸ÐºÐ¾Ð²Ð°Ñ Ð·Ð²ÐµÐ·Ð´Ð° Ð³Ð»Ð°Ð²Ð½Ð¾Ð¹ Ð¿Ð¾ÑÐ»ÐµÐ´Ð¾Ð²Ð°ÑÐµÐ»ÑÐ½Ð¾ÑÑÐ¸, ÑÑÐ¾ Ð¿Ð¾Ð»ÑÑÐ¸Ð»Ð¾ Ð¿Ð¾Ð»Ð½Ð¾Ðµ ÑÐ¾Ð³Ð»Ð°ÑÐ¾Ð²Ð°Ð½Ð¸Ðµ Ñ ÑÐµÐ·ÑÐ»ÑÑÐ°ÑÐ°Ð¼Ð¸ ÑÐ°Ð±Ð¾ÑÑ Edmonds et al, Ð¿ÑÐ¾Ð¸Ð·Ð²ÐµÐ´ÐµÐ½Ð½Ð¾Ð¹ Ð² 2002 Ð³Ð¾Ð´Ñ. Ð ÑÐ°ÐºÐ¶Ðµ Ð¿Ð¾Ð·Ð²Ð¾Ð»Ð¸Ð»Ð¾ Ð¿ÑÐ¾Ð¸Ð·Ð²ÐµÑÑÐ¸ ÑÐ°ÑÑÐµÑ Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÐ¾Ð² Ð´Ð²Ð¾Ð¹Ð½Ð¾Ð¹ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð¹ ÑÐ¸ÑÑÐµÐ¼Ñ Ñ5: Ð¼Ð°ÑÑÑ, ÑÑÑÐµÐºÑÐ¸Ð²Ð½Ð¾Ð¹ ÑÐµÐ¼Ð¿ÐµÑÐ°ÑÑÑÑ Ð¿Ð¾Ð²ÐµÑÑÐ½Ð¾ÑÑÐ¸ Ð¸ ÑÐ°Ð´Ð¸ÑÑÐ° Ð¾Ð¿ÑÐ¸ÑÐµÑÐºÐ¾Ð³Ð¾ ÐºÐ¾Ð¼Ð¿Ð°Ð½ÑÐ¾Ð½Ð°, Ð° ÑÐ°ÐºÐ¶Ðµ Ð±Ð¾Ð»ÑÑÐ¾Ð¹ Ð¿Ð¾Ð»ÑÐ¾ÑÐ¸ Ð´Ð²Ð¾Ð¹Ð½Ð¾Ð¹ ÑÐ¸ÑÑÐµÐ¼Ñ, ÑÐ°Ð·Ð¼ÐµÑÐ¾Ð² Ð¿Ð¾Ð»Ð¾ÑÑÐ¸ Ð Ð¾ÑÐ° Ð¸ Ð¿ÑÐ¾ÑÐµÐ½ÑÐ° ÐµÑ Ð·Ð°Ð¿Ð¾Ð»Ð½ÐµÐ½Ð¸Ñ. Ð¢ÐµÐ¼ Ð½Ðµ Ð¼ÐµÐ½ÐµÐµ, Ð¿Ð¾Ð»Ð¾Ð¶ÐµÐ½Ð¸Ðµ Ð²Ð¾Ð·Ð¼Ð¾Ð¶Ð½ÑÑ ÐºÐ¾Ð¼Ð¿Ð¾Ð½ÐµÐ½ÑÐ¾Ð² ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð¹ ÑÐ¸ÑÑÐµÐ¼Ñ Ñ7 (N1, N2) Ð½Ð° Ð´Ð¸Ð°Ð³ÑÐ°Ð¼Ð¼Ðµ Ð¦Ð²ÐµÑ-ÐÐ²ÐµÐ·Ð´Ð½Ð°Ñ Ð²ÐµÐ»Ð¸ÑÐ¸Ð½Ð°, Ð¸ÑÑÐ¾Ð´Ñ Ð¸Ð· Ð°Ð½Ð°Ð»Ð¸Ð·Ð° Ð¿Ð¾Ð»ÑÑÐµÐ½Ð½Ð¾Ð³Ð¾ Ð½Ð°Ð±Ð¾ÑÐ° Ð´Ð°Ð½Ð½ÑÑ, Ð² Ð´Ð¾ÑÑÐ°ÑÐ¾ÑÐ½Ð¾Ð¹ Ð¼ÐµÑÐµ Ð½Ðµ Ð¿Ð¾Ð·Ð²Ð¾Ð»ÑÐµÑ ÐºÐ»Ð°ÑÑÐ¸ÑÐ¸ÑÐ¸ÑÐ¾Ð²Ð°ÑÑ Ð¾Ð±Ð½Ð°ÑÑÐ¶ÐµÐ½Ð½ÑÐµ Ð²Ð¾Ð·Ð¼Ð¾Ð¶Ð½ÑÐµ Ð¾Ð¿ÑÐ¸ÑÐµÑÐºÐ¸Ðµ ÐºÐ¾Ð¼Ð¿Ð°Ð½ÑÐ¾Ð½Ñ ÑÐ¸ÑÑÐµÐ¼Ñ Ñ7 (N1, N2). ÐÐ»Ñ Ð¿Ð¾Ð½Ð¸Ð¼Ð°Ð½Ð¸Ñ Ð¿ÑÐ¸ÑÐ¾Ð´Ñ ÐºÐ¾ÑÐ¾ÑÐ¾Ð¹, Ð½ÐµÐ¾Ð±ÑÐ¾Ð´Ð¸Ð¼Ð¾ Ð¿ÑÐ¾Ð²ÐµÑÑÐ¸ Ð´Ð¾Ð¿Ð¾Ð»Ð½Ð¸Â­ ÑÐµÐ»ÑÐ½ÑÐµ Ð½Ð°Ð±Ð»ÑÐ´ÐµÐ½Ð¸Ñ ÐºÐ°Ðº Ð² Ð±Ð»Ð¸Ð¶Ð½ÐµÐ¼ Ð¸Ð½ÑÑÐ°ÐºÑÐ°ÑÐ½Ð¾Ð¼, ÑÐ°Ðº Ð¸ Ð² ÑÐ»ÑÑÑÐ°ÑÐ¸Ð¾Ð»ÐµÑÐ¾Ð²Ð¾Ð¼ Ð´Ð¸Ð°Ð¿Ð°Ð·Ð¾Ð½Ð°Ñ. Ð§ÑÐ¾ Ð¿Ð¾Ð¼Ð¾Ð¶ÐµÑ ÑÐ¾ÑÐ½ÑÐ¼ Ð¾Ð±ÑÐ°Ð·Ð¾Ð¼ Ð¾Ð¿ÑÐµÐ´ÐµÐ»Ð¸ÑÑ ÑÐ¿ÐµÐºÑÑÐ°Ð»ÑÐ½ÑÐ¹ ÐºÐ»Ð°ÑÑ Ð¸Ð·ÑÑÐ°ÐµÐ¼Ð¾Ð¹ ÑÐ¸ÑÑÐµÐ¼Ñ, Ð° ÑÐ°ÐºÐ¶Ðµ ÑÐ¸Ð·Ð¸ÑÐµÑÐºÐ¸Ðµ Ð¿ÑÐ¾ÑÐµÑÑÑ, Ð¿ÑÐ¾ÑÐµÐºÐ°ÑÑÐ¸Ðµ Ð² ÐµÑ Ð³ÑÐ°Ð½Ð¸ÑÐ°Ñ.
description: The given work is devoted to studying of the quiescent low-mass X-ray binaries X5 and X7 in the globular cluster 47 Tucanae. Data analysis was carried out based on scientific data from the studied globular cluster observed by two observatories in different exposures and filters: Gemini GSAOI â series of images in the infrared spectral range ( Ks and J filters in 30 and 60 exposures); Hubble Space Telescope (HST) â series of images in the optical part of the spectrum (F275W, F336W, F438W, F555W, F606W, F814W filters in high-exposure times). Each of the observed systems is plotted on Colour Magnitude Diagram (CMD), drawn for a globular cluster NGC 104 in two sets of filters: F606W, F814W (based on project HUGS database) and F555W,Ks (based on aggregate data of two observatories). Based on the obtained dependences, it was concluded that the secondary low mass companion of two different systems belongs to the main sequence stars (MSS). The position of the optical companion of the x5 X-ray source on the Hertzsprungâ Russell diagram made it possible to determine its spectral type - a main sequence dwarf star, which was in full agreement with the results of the work by Edmonds et al, performed in 2002. It also made it possible to calculate the parameters of the double x-ray system x5: mass, effective surface temperature and radius of the optical companion, as well as the semi-major axis of the binary system, the size of the Roche lobe and the percentage of its filling. However, the position of the possible components of the X-ray system x7 (N1, N2) ploted on the Colour-Magnitude Diagram, based on the analysis of the obtained data set, it does not sufficiently allow classifying the detected possible optical companions of the x7 (N1, N2) system. To understand the nature of which, it is necessary to carry out additional observations in both the near infrared and ultraviolet ranges. This will help to accurately determine the spectral type of the studied system, as well as the physical processes occurring within its boundaries.