Repeating X-ray bursts: Interaction between a neutron star and clumps partially disrupted from a planet

Open Access

Table 1.

Typical parameters of the planets considered in our study and the timing parameters of the clumps originated from the inner side of the planet.

m_pl	R_pl	$\frac{m_{pl}}{R_{pl}}$ $\frac{m_{\mathrm{pl}}}{R_{\mathrm{pl}}}$	$P_{orb}^{cl}$ $P_{\mathrm{orb}}^{\mathrm{cl}}$	t_trav	$P_{orb, c}^{cl}$ $P_{\mathrm{orb,c}}^{\mathrm{cl}}$	t_trav, c	$Δ P_{orb, up}^{cl}$ $\Delta P_{\mathrm{orb,up}}^{\mathrm{cl}}$	Δt_trav, up	$P_{orb}^{cl}$ $P_{\mathrm{orb}}^{\mathrm{cl}}$	t_trav	$P_{orb, c}^{cl}$ $P_{\mathrm{orb,c}}^{\mathrm{cl}}$	t_trav, c	$Δ P_{orb, up}^{cl}$ $\Delta P_{\mathrm{orb,up}}^{\mathrm{cl}}$	Δt_trav, up
			P_orb = 238 days						P_orb = 398 days

(M_⊕)	(R_⊕)	(days)	(days)	(days)	(days)	(days)	(days)	(days)	(days)	(days)	(days)	(days)	(days)
Fe planet
4.6	1.2	3.8	36.3	73.1	115.1	230.3	78.8	157.2	41.3	83.1	154.7	309.4	113.3	226.3
10.1	1.4	7.2	24.6	49.6	92.4	184.9	67.8	135.3	27.2	54.7	118.9	237.8	91.6	183.1
18.1	1.6	11.1	17.9	35.9	75.6	151.3	57.8	115.4	19.3	38.8	94.0	188.0	74.7	149.2

MgSiO₃ planet

4.4	1.7	2.6	54.9	111.1	141.7	283.8	86.8	172.8	65.3	131.6	200.1	400.5	134.8	268.8
9.9	2.1	4.7	40.1	80.8	121.4	242.9	81.3	162.0	46.0	92.7	165.0	330.1	119.0	237.4
18.2	2.5	7.3	30.8	62.1	105.3	210.8	74.5	148.7	34.6	69.6	138.9	277.9	104.3	208.3

Two-layer planet

3.3	1.4	2.4	53.8	108.7	140.4	281.0	86.5	172.3	63.8	128.6	197.7	395.5	133.8	267.0
9.8	1.8	5.4	34.4	69.4	112.0	224.0	77.5	154.6	39.0	78.5	149.6	299.2	110.5	220.7
12.8	1.6	8.0	24.0	48.3	91.0	181.9	67.0	133.7	26.4	53.1	116.6	233.3	90.2	180.2
17.1	2.4	7.1	31.1	62.6	105.8	211.7	74.7	149.1	34.9	70.2	139.6	279.3	104.8	209.2

Notes. The timing parameters of the clumps are calculated for two cases of the planet’s orbital period (P_orb = 238, 398 days) according to the methods given in the main text.

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